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{{Short description|Periodic table of the elements with 8 or more periods}}

{{Periodic table (micro)|number=119|mark=Uue|title=Extended periodic table|caption= Element 119 ([[Ununennium|Uue]], marked here) in period 8 (row 8) marks the start of theorisations.}}
{{Sidebar periodic table|expanded=forms}}

An '''extended [[periodic table]]''' theorizes about [[chemical elements]] beyond those currently known and proven. The element with the highest [[atomic number]] known is [[oganesson]] (''Z'' = 118), which completes the seventh [[period (periodic table)|period]] (row) in the [[periodic table]]. All elements in the eighth period and beyond thus remain purely hypothetical.

Elements beyond 118 will be placed in additional periods when discovered, laid out (as with the existing periods) to illustrate periodically recurring trends in the properties of the elements. Any additional periods are expected to contain more elements than the seventh period, as they are calculated to have an additional so-called ''g-block'', containing at least 18 elements with partially filled g-[[atomic orbital|orbitals]] in each period. An ''eight-period table'' containing this block was suggested by [[Glenn T. Seaborg]] in 1969.<ref name=LBL>{{cite web|url=http://www.lbl.gov/LBL-PID/Nobelists/Seaborg/65th-anniv/29.html|title=An Early History of LBNL|first=Glenn T.|last=Seaborg|author-link=Glenn T. Seaborg|date=August 26, 1996|access-date=2011-02-25|archive-date=2010-11-15|archive-url=https://web.archive.org/web/20101115025829/http://www.lbl.gov/LBL-PID/Nobelists/Seaborg/65th-anniv/29.html|url-status=dead}}</ref><ref name=SHE78>{{cite journal | doi = 10.2307/3963006 | last1 = Frazier | first1 = K. | title = Superheavy Elements | journal = Science News | volume = 113 | issue = 15 | pages = 236–238 | year = 1978 | jstor = 3963006}}</ref> The first element of the g-block may have atomic number 121, and thus would have the [[Systematic element name|systematic name]] [[unbiunium]]. Despite many searches, no elements in this region have been [[Synthetic element|synthesized]] or discovered in nature.<ref>[[Unbibium|Element 122]] was claimed to exist naturally in April 2008, but this claim was widely believed to be erroneous. {{cite web|url=http://www.rsc.org/chemistryworld/News/2008/May/02050802.asp|title=Heaviest element claim criticised|publisher=Rsc.org|date=2008-05-02|access-date=2010-03-16}}</ref>

According to the orbital approximation in [[quantum mechanics|quantum mechanical]] descriptions of atomic structure, the g-block would correspond to elements with partially filled g-orbitals, but [[spin–orbit coupling]] effects reduce the validity of the orbital approximation substantially for elements of high atomic number. Seaborg's version of the extended period had the heavier elements following the pattern set by lighter elements, as it did not take into account [[relativistic quantum chemistry|relativistic effects]]. Models that take relativistic effects into account predict that the pattern will be broken. [[Pekka Pyykkö]] and [[Burkhard Fricke]] used computer modeling to calculate the positions of elements up to ''Z'' = 172, and found that several were displaced from the [[Aufbau principle#Madelung energy ordering rule|Madelung rule]].<ref name="Fricke">{{cite journal |last1=Fricke |first1=B. |last2=Greiner |first2=W. |last3=Waber |first3=J. T. |year=1971 |title=The continuation of the periodic table up to Z = 172. The chemistry of superheavy elements |journal=Theoretica Chimica Acta |volume=21 |issue=3 |pages=235–260 |doi=10.1007/BF01172015|s2cid=117157377 }}</ref> As a result of uncertainty and variability in predictions of chemical and physical properties of elements beyond 120, there is currently no consensus on their placement in the extended periodic table.

Elements in this region are likely to be highly unstable with respect to [[radioactive decay]] and undergo [[alpha decay]] or [[spontaneous fission]] with extremely short [[half-life|half-lives]], though [[unbihexium|element 126]] is hypothesized to be within an [[island of stability]] that is resistant to fission but not to alpha decay. Other islands of stability beyond the known elements may also be possible, including one theorised around element 164, though the extent of stabilizing effects from closed [[nuclear shell model|nuclear shells]] is uncertain. It is not clear how many elements beyond the expected island of stability are physically possible, whether period 8 is complete, or if there is a period 9. The [[International Union of Pure and Applied Chemistry]] (IUPAC) defines an element to exist if its lifetime is longer than 10−14 seconds (0.01 picoseconds, or 10 femtoseconds), which is the time it takes for the nucleus to form an [[electron cloud]].<ref>{{Cite web|url=http://www.kernchemie.de/Transactinides/Transactinide-2/transactinide-2.html|title=Kernchemie|website=www.kernchemie.de|access-date=2014-11-09}}</ref>

As early as 1940, it was noted that a simplistic interpretation of the [[Theory of relativity|relativistic]] [[Dirac equation]] runs into problems with electron orbitals at ''Z''&nbsp;>&nbsp;1/α&nbsp;≈&nbsp;137, suggesting that neutral atoms cannot exist beyond element 137, and that a periodic table of elements based on electron orbitals therefore breaks down at this point.<ref>{{cite journal|last1=Schiff |first1=L. I. |last2=Snyder |first2=H. |last3=Weinberg |first3=J. |title=On the Existence of Stationary States of the Mesotron Field |journal=[[Physical Review]] |volume=57 |issue=4 |pages=315–318 |year=1940 |doi=10.1103/PhysRev.57.315|bibcode=1940PhRv...57..315S }}</ref> On the other hand, a more rigorous analysis calculates the analogous limit to be ''Z''&nbsp;≈&nbsp;168–172 where the 1s subshell dives into the [[Dirac sea]], and that it is instead not neutral atoms that cannot exist beyond this point, but bare nuclei, thus posing no obstacle to the further extension of the periodic system. Atoms beyond this critical atomic number are called ''supercritical'' atoms.

==History==
Elements beyond the [[actinide]]s were first proposed to exist as early as 1895, when Danish chemist [[Hans Peter Jørgen Julius Thomsen]] predicted that [[thorium]] and [[uranium]] formed part of a 32-element period which would end at a chemically inactive element with atomic weight 292 (not far from the 294 for the only known isotope of [[oganesson]]). In 1913, Swedish physicist [[Johannes Rydberg]] similarly predicted that the next noble gas after [[radon]] would have atomic number 118, and purely formally derived even heavier congeners of radon at ''Z''&nbsp;=&nbsp;168, 218, 290, 362, and 460, exactly where the [[Aufbau principle]] would predict them to be. [[Niels Bohr]] predicted in 1922 the electronic structure of this next [[noble gas]] at ''Z''&nbsp;=&nbsp;118, and suggested that the reason why elements beyond uranium were not seen in nature was because they were too unstable. The German physicist and engineer Richard Swinne published a review paper in 1926 containing predictions on the [[transuranic element]]s (he may have coined the term) in which he anticipated modern predictions of an [[island of stability]]: he first hypothesised in 1914 that half-lives should not decrease strictly with atomic number, but suggested instead that there might be some longer-lived elements at ''Z''&nbsp;=&nbsp;98–102 and ''Z''&nbsp;=&nbsp;108–110, and speculated that such elements might exist in the [[Earth's core]], in [[iron meteorites]], or in the [[Greenland ice sheet|ice caps of Greenland]] where they had been locked up from their supposed cosmic origin.<ref>{{cite book |last=Kragh |first=Helge |date=2018 |title=From Transuranic to Superheavy Elements: A Story of Dispute and Creation |publisher=Springer |pages=6–10 |isbn=9783319758138}}</ref> By 1955, these elements were called ''superheavy'' elements.<ref name=Transuraniumppl />

The first predictions on properties of undiscovered superheavy elements were made in 1957, when the concept of [[nuclear shell model|nuclear shells]] was first explored and an island of stability was theorized to exist around element&nbsp;126.<ref name=fossilfission /> In 1967, more rigorous calculations were performed, and the island of stability was theorized to be centered at the then-undiscovered [[flerovium]] (element 114); this and other subsequent studies motivated many researchers to search for superheavy elements in nature or attempt to [[synthetic element|synthesize]] them at accelerators.<ref name=Transuraniumppl /> Many searches for superheavy elements were conducted in the 1970s, all with negative results. {{As of|2022|4}}, synthesis has been attempted for every element up to and including unbiseptium (''Z''&nbsp;=&nbsp;127), except unbitrium (''Z''&nbsp;=&nbsp;123),<ref name="emsley" /><ref name=beyonduranium /><ref name=superlourds /> with the heaviest successfully synthesized element being [[oganesson]] in 2002 and the most recent discovery being that of [[tennessine]] in 2010.<ref name="emsley" />

As some superheavy elements were predicted to lie beyond the seven-period periodic table, an additional eighth period containing these elements was first proposed by [[Glenn T. Seaborg]] in 1969. This model continued the pattern in established elements and introduced a new g-block and superactinide series beginning at element&nbsp;121, raising the number of elements in period 8 compared to known periods.<ref name=LBL /><ref name=SHE78 /><ref name=Transuraniumppl /> These early calculations failed to consider relativistic effects that break down periodic trends and render simple extrapolation impossible, however. In 1971, Fricke calculated the periodic table up to ''Z''&nbsp;=&nbsp;172, and discovered that some elements indeed had different properties that break the established pattern,<ref name="Fricke" /> and a 2010 calculation by [[Pekka Pyykkö]] also noted that several elements might behave differently than expected.<ref name="PT172" /> It is unknown how far the periodic table might extend beyond the known 118 elements, as heavier elements are predicted to be increasingly unstable. [[Glenn T. Seaborg]] suggested that practically speaking, the end of the periodic table might come as early as around ''Z''&nbsp;=&nbsp;120 due to nuclear instability.<ref name=EB/>

==Predicted structures of an extended periodic table==
There is currently no consensus on the placement of elements beyond [[unbinilium|atomic number 120]] in the periodic table.

All hypothetical elements are given an [[International Union of Pure and Applied Chemistry]] (IUPAC) [[systematic element name]], for use until the element has been discovered, confirmed, and an official name is approved. These names are typically not used in the literature, and the elements are instead referred to by their atomic numbers; hence, element 164 is usually not called "unhexquadium" or "Uhq" (the systematic name and symbol), but rather "element 164" with symbol "164", "(164)", or "E164".<ref name=Haire/>

===Aufbau principle===
At element 118, the orbitals 1s, 2s, 2p, 3s, 3p, 3d, 4s, 4p, 4d, 4f, 5s, 5p, 5d, 5f, 6s, 6p, 6d, 7s and 7p are assumed to be filled, with the remaining orbitals unfilled. A simple extrapolation from the [[Aufbau principle]] would predict the eighth row to fill orbitals in the order 8s, 5g, 6f, 7d, 8p; but after element 120, the proximity of the electron shells makes placement in a simple table problematic.
{{Extended periodic table (by Aufbau, 50 columns, compact)}}

===Fricke===
Not all models show the higher elements following the pattern established by lighter elements. Burkhard Fricke et al., who carried out calculations up to element 184 in an article published in 1971, also found some elements to be displaced from the [[Aufbau principle|Madelung energy-ordering rule]] as a result of overlapping orbitals; this is caused by the increasing role of [[relativistic quantum chemistry|relativistic effects]] in heavy elements (They describe chemical properties up to element 184, but only draw a table to element 172.)<ref name="Fricke"/><ref name="BFricke" />
{| class="wikitable" style="text-align: center;"
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| V
| Cr
| Mn
| Fe
| Co
| Ni
| Cu
| Zn
| Ga
| Ge
| As
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| Br
| Kr
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| Rb
| Sr
| Y
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| Zr
| Nb
| Mo
| Tc
| Ru
| Rh
| Pd
| Ag
| Cd
| In
| Sn
| Sb
| Te
| I
| Xe
|-
| Cs
| Ba
| La
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| Ce–Lu
| Hf
| Ta
| W
| Re
| Os
| Ir
| Pt
| Au
| Hg
| Tl
| Pb
| Bi
| Po
| At
| Rn
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| Fr
| Ra
| Ac
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| Th–Lr
| Rf
| Db
| Sg
| Bh
| Hs
| Mt
| Ds
| Rg
| Cn
| Nh
| Fl
| Mc
| Lv
| Ts
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| 119
| 120
| 121
| {{nowrap|122–141}}
| 142–155
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Fricke et al.'s format is more focused on formal electron configurations than likely chemical behaviour. They place elements 156–164 in groups 4–12 because formally their configurations should be 7d2 through 7d10. However, they differ from the previous d-elements in that the 8s shell is not available for chemical bonding: instead, the 9s shell is. Thus element 164 with 7d109s0 is noted by Fricke et al. to be analogous to palladium with 4d105s0, and they consider elements 157–172 to have chemical analogies to groups 3–18 (though they are ambivalent on whether elements 165 and 166 are more like group 1 and 2 elements or more like group 11 and 12 elements, respectively). Thus, elements 157–164 are placed in their table in a group that the authors do not think is chemically most analogous.<ref name=actrev>{{cite journal |last1=Fricke |first1=Burkhard |last2=Waber |first2=J. T. |date=1971 |title=Theoretical Predictions of the Chemistry of Superheavy Elements: Continuation of the Periodic Table up to Z{{=}}184 |url=https://kobra.uni-kassel.de/bitstream/handle/123456789/2008100124269/Fricke_theoretical_1971.pdf |journal=Actinides Reviews |volume=1 |issue= |pages=433–485 |doi= |access-date=5 January 2024}}</ref>

===Nefedov===
{{ill|Vadim Nefedov|lt=Nefedov|ru|Нефёдов, Вадим Иванович}}, Trzhaskovskaya, and Yarzhemskii carried out calculations up to 164 (results published in 2006). They considered elements 158 through 164 to be homologues of groups 4 through 10, and not 6 through 12, noting similarities of electron configurations to the period 5 transition metals (e.g. element 159 7d49s1 vs Nb 4d45s1, element 160 7d59s1 vs Mo 4d55s1, element 162 7d79s1 vs Ru 4d75s1, element 163 7d89s1 vs Rh 4d85s1, element 164 7d109s0 vs Pd 4d105s0). They thus agree with Fricke et al. on the chemically most analogous groups, but differ from them in that Nefedov et al. actually place elements in the chemically most analogous groups. Rg and Cn are given an asterisk to reflect differing configurations from Au and Hg (in the original publication they are drawn as being displaced in the third dimension). In fact Cn probably has an analogous configuration to Hg, and the difference in configuration between Pt and Ds is not marked.<ref name=nefedov/>
{| class="wikitable" style="text-align: center;"
|+Nefedov et al.'s suggested form (fragment)
|-
| Cs
| Ba
| La–Lu
| Hf
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| W
| Re
| Os
| Ir
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| Au
| Hg
| Tl
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| Bi
| Po
| At
| Rn
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| Fr
| Ra
| Ac–Lr
| Rf
| Db
| Sg
| Bh
| Hs
| Mt
| Ds
| Rg*
| Cn*
| Nh
| Fl
| Mc
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| Og
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| 119
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| {{nowrap|121–157}}

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===Pyykkö===
[[Pekka Pyykkö]] used computer modeling to calculate the positions of elements up to ''Z''&nbsp;=&nbsp;172 and their possible chemical properties in an article published in 2011. He reproduced the orbital order of Fricke et al., and proposed a refinement of their table by formally assigning slots to elements 121–164 based on ionic configurations.<ref name="PT172">{{Cite journal|last1=Pyykkö|first1=Pekka|s2cid=31590563|author-link=Pekka Pyykkö|title=A suggested periodic table up to Z≤ 172, based on Dirac–Fock calculations on atoms and ions|journal=Physical Chemistry Chemical Physics|volume=13|issue=1|pages=161–8|year=2011|pmid=20967377|doi=10.1039/c0cp01575j|bibcode = 2011PCCP...13..161P }}</ref>
[[File:Pyykko periodic table 172.svg|thumb|center|512px]]
In order to bookkeep the electrons, Pyykkö places some elements out of order: thus 139 and 140 are placed in groups 13 and 14 to reflect that the 8p1/2 shell needs to fill, and he distinguishes separate {{not a typo|5g}}, 8p1/2, and 6f series.<ref name=PT172/> Fricke et al. and Nefedov et al. do not attempt to break up these series.<ref name=actrev/><ref name=nefedov/>

===Kulsha===
Computational chemist [[Andrey Kulsha]] has suggested two forms of the extended periodic table up to 172 that build on and refine Nefedov et al.'s versions up to 164 with reference to Pyykkö's calculations.<ref name=primefan/> Based on their likely chemical properties, elements 157–172 are placed by both forms as eighth-period congeners of yttrium through xenon in the fifth period;<ref name=primefan/> this extends Nefedov et al.'s placement of 157–164 under yttrium through palladium,<ref name=nefedov>{{cite journal |last1=Nefedov |first1=V.I. |last2=Trzhaskovskaya |first2=M.B. |last3=Yarzhemskii |first3=V.G. |title=Electronic Configurations and the Periodic Table for Superheavy Elements |journal=Doklady Physical Chemistry |date=2006 |volume=408 |issue=2 |pages=149–151 |doi=10.1134/S0012501606060029 |s2cid=95738861 |issn=0012-5016 |url=http://www.primefan.ru/stuff/chem/nefedov.pdf}}</ref> and agrees with the chemical analogies given by Fricke et al.<ref name=actrev/>

Kulsha suggested two ways to deal with elements 121–156, that lack precise analogues among earlier elements. In his first form (2011, after Pyykkö's paper was published),<ref name=primefan/> elements 121–138 and 139–156 are placed as two separate rows (together called "ultransition elements"), related by the addition of a 5g18 subshell into the core, as according to Pyykkö's calculations of oxidation states,<ref name=PT172/> they should respectively mimic lanthanides and actinides.<ref name=primefan/><ref name=sicius>{{cite book |last=Sicius |first=Hermann |author-link= |date=2021 |title=Handbuch der chemischen Elemente |language=de |url= |location= |publisher=Springer |page=1085 |isbn= |quote=Kulsha nennt die 36 Elemente zwischen 121 und 156 „Ultransition Elements“ und schlägt vor, sie in zwei Serien aufzuteilen, in eine von 121 bis 138 und eine zweite von 139 bis 156. Die erste ähnelte eher den Lanthanoiden (Seltenerden), die zweite mehr den Actinoiden.}}</ref> In his second suggestion (2016), elements 121–142 form a g-block (as they have 5g activity), while elements 143–156 form an f-block placed under actinium through nobelium.<ref name=dications/>
[[File:Pt172.svg|center|512px|thumb|Kulsha's first suggested form]]
[[File:Pt172expanded.svg|center|1024px|thumb|Kulsha's second suggested form]]
Thus, period 8 emerges with 54 elements, and the next noble element after 118 is 172.<ref name=wothers>{{cite book |last=Wothers |first=Peter |author-link= |date=2019 |title=Antimony, Gold, and Jupiter's Wolf |url= |location= |publisher=Oxford University Press |page=vii |isbn=978-0-19-965272-3 |quote=It’s possible that other elements might be synthesized—research is certainly ongoing—but it’s unlikely that the table will ever appear as neat again, since to fill the next row, another fifty-four elements would need to be made.}}</ref>

===Smits et al.===
In 2023 Smits, Düllmann, Indelicato, Nazarewicz, and Schwerdtfeger made another attempt to place elements from 119 to 170 in the periodic table based on their electron configurations. A few elements (121–124 and 168) could not be placed unambiguously. {{why|date=May 2024}} Element 145 appears twice, some places have double occupancy, and others are empty.<ref>{{cite journal |last1=Smits |first1=Odile R. |last2=Düllmann |first2=Christoph E. |last3=Indelicato |first3=Paul |last4=Nazarewicz |first4=Witold |last5=Schwerdtfeger |first5=Peter |date=2023 |title=The quest for superheavy elements and the limit of the periodic table |url= |journal=Nature Reviews Physics |volume= 6|issue= 2|pages= 86–98|doi=10.1038/s42254-023-00668-y |access-date=}}</ref>

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| Dy
| Ho
| Er
| Tm
| Yb
| Lu
| Hf
| Ta
| W
| Re
| Os
| Ir
| Pt
| Au
| Hg
| Tl
| Pb
| Bi
| Po
| At
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| Fr
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| Ac
| Th
| Pa
| U
| Np
| Pu
| Am
| Cm
| Bk
| Cf
| Es
| Fm
| Md
| No
| Lr
| Rf
| Db
| Sg
| Bh
| Hs
| Mt
| Ds
| Rg
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| 119
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==Searches for undiscovered elements==
===Synthesis attempts===
Unsuccessful attempts have been made to synthesise the period 8 elements up to unbiseptium, except unbitrium. Attempts to synthesise ununennium, the first period 8 element, are ongoing {{as of|{{CURRENTYEAR}}|lc=y}}.

==== Ununennium (E119) ====
{{Main|Ununennium#Synthesis attempts}}
The synthesis of element 119 ([[ununennium]]) was first attempted in 1985 by bombarding a target of einsteinium-254 with [[calcium-48]] ions at the superHILAC accelerator at Berkeley, California:

:{{nuclide|einsteinium|254}} + {{nuclide|calcium|48}} → {{sup|302}}119* → no atoms

No atoms were identified, leading to a limiting [[cross section (physics)|cross section]] of 300 [[barn (unit)|nb]].<ref>{{cite journal|title=Search for superheavy elements using 48Ca + 254Esg reaction|journal=Physical Review C|date=1985|pages=1760–1763|doi=10.1103/PhysRevC.32.1760|pmid=9953034|volume=32|issue=5|bibcode = 1985PhRvC..32.1760L|last1=Lougheed|first1=R.|last2=Landrum|first2=J.|last3=Hulet|first3=E.|last4=Wild|first4=J.|last5=Dougan|first5=R.|last6=Dougan|first6=A.|last7=Gäggeler|first7=H.|last8=Schädel|first8=M.|last9=Moody|first9=K.|display-authors=1}}</ref> Later calculations suggest that the cross section of the 3n reaction (which would result in {{sup|299}}119 and three neutrons as products) would actually be six hundred thousand times lower than this upper bound, at 0.5&nbsp;pb.<ref>{{cite journal|arxiv=0803.1117|doi=10.1016/j.nuclphysa.2008.11.003|title=Production of heavy and superheavy nuclei in massive fusion reactions|date=2009|author=Feng, Z|journal=Nuclear Physics A|volume=816|issue=1|page=33|last2=Jin|first2=G.|last3=Li|first3=J.|last4=Scheid|first4=W.|bibcode=2009NuPhA.816...33F|s2cid=18647291}}</ref>

From April to September 2012, an attempt to synthesize the isotopes {{sup|295}}119 and {{sup|296}}119 was made by bombarding a target of [[berkelium]]-249 with [[titanium]]-50 at the [[GSI Helmholtz Centre for Heavy Ion Research]] in [[Darmstadt]], Germany.<ref name="economist">[http://www.economist.com/node/21554502 Modern alchemy: Turning a line], [[The Economist]], May 12, 2012.</ref><ref name=Khuyagbaatar>[http://asrc.jaea.go.jp/soshiki/gr/chiba_gr/workshop2/&Khuyagbaatar.pdf Superheavy Element Search Campaign at TASCA]. J. Khuyagbaatar</ref> Based on the theoretically predicted cross section, it was expected that an ununennium atom would be synthesized within five months of the beginning of the experiment.<ref name=Zagrebaev>{{cite journal|title=Future of superheavy element research: Which nuclei could be synthesized within the next few years?|url=http://nrv.jinr.ru/pdf_file/J_phys_2013.pdf|first1=Valeriy|last1=Zagrebaev|first2=Alexander|last2=Karpov|first3=Walter|last3=Greiner|date=2013|journal=Journal of Physics|volume=420|issue=1|pages=012001|doi=10.1088/1742-6596/420/1/012001|arxiv=1207.5700|bibcode=2013JPhCS.420a2001Z|s2cid=55434734}}</ref> Moreover, as berkelium-249 decays to [[californium]]-249 (the next element) with a short half-life of 327&nbsp;days, this allowed elements 119 and 120 to be searched for simultaneously.<ref name="search">{{cite journal |last1=Khuyagbaatar |first1=J. |last2=Yakushev |first2=A. |last3=Düllmann |first3=Ch. E. |display-authors=etal |date=2020 |title=Search for elements 119 and 120 |url=https://jyx.jyu.fi/bitstream/handle/123456789/73027/2/khuyagbaatarym0812.pdf |journal=Physical Review C |volume=102 |issue=6 |at=064602 |doi=10.1103/PhysRevC.102.064602 |bibcode=2020PhRvC.102f4602K |hdl=1885/289860 |s2cid=229401931 |access-date=25 January 2021}}</ref>

:{{nuclide|berkelium|249}} + {{nuclide|titanium|50}} → {{sup|299}}119* → no atoms

The experiment was originally planned to continue to November 2012,<ref>{{Cite web |url=https://www-win.gsi.de/tasca12/program/contributions/TASCA12_Duellmann.pdf |title=Search for element 119: Christoph E. Düllmann for the ''TASCA E119'' collaboration |access-date=2017-04-05 |archive-url=https://web.archive.org/web/20160304094201/https://www-win.gsi.de/tasca12/program/contributions/TASCA12_Duellmann.pdf |archive-date=2016-03-04 |url-status=dead }}</ref> but was stopped early to make use of the {{sup|249}}Bk target to confirm the synthesis of [[tennessine]] (thus changing the projectiles to {{sup|48}}Ca).<ref name=Yakushev/> This reaction between {{sup|249}}Bk and {{sup|50}}Ti was predicted to be the most favorable practical reaction for formation of element 119,<ref name=Khuyagbaatar/> as it is rather asymmetrical,<ref name=Zagrebaev/> though also somewhat cold.<ref name=Yakushev/> (The reaction between {{sup|254}}Es and {{sup|48}}Ca would be superior, but preparing milligram quantities of {{sup|254}}Es for a target is difficult.)<ref name=Zagrebaev/> Nevertheless, the necessary change from the "silver bullet" {{sup|48}}Ca to {{sup|50}}Ti divides the expected yield of element 119 by about twenty, as the yield is strongly dependent on the asymmetry of the fusion reaction.<ref name=Zagrebaev/>

Due to the predicted short half-lives, the GSI team used new "fast" electronics capable of registering decay events within microseconds.<ref name=Khuyagbaatar/> No atoms of element 119 were identified, implying a limiting cross section of 70&nbsp;fb.<ref name=Yakushev/> The predicted actual cross section is around 40&nbsp;fb, which is at the limits of current technology.<ref name=Zagrebaev/>

The team at RIKEN in [[Wakō, Saitama|Wakō]], Japan began bombarding [[curium]]-248 targets with a [[vanadium]]-51 beam in January 2018<ref name=sakai22>{{cite journal |last1=Sakai |first1=Hideyuki |last2=Haba |first2=Hiromitsu |first3=Kouji |last3=Morimoto |first4=Naruhiko |last4=Sakamoto |date=9 December 2022 |title=Facility upgrade for superheavy-element research at RIKEN |journal=The European Physical Journal A |volume=58 |issue=238 |page=238 |doi=10.1140/epja/s10050-022-00888-3 |pmid=36533209 |pmc=9734366 |bibcode=2022EPJA...58..238S }}</ref> to search for element 119. Curium was chosen as a target, rather than heavier berkelium or californium, as these heavier targets are difficult to prepare.<ref name="sakai">{{cite web |url=http://www0.mi.infn.it/~colo/slides_27_2_19/2019-2_Milano-WS_sakai.pdf |title=Search for a New Element at RIKEN Nishina Center |last=Sakai |first=Hideyuki |date=27 February 2019 |website=infn.it |access-date=17 December 2019}}</ref> The 248Cm targets were provided by [[Oak Ridge National Laboratory]]. RIKEN developed a high-intensity vanadium beam.<ref name=usprogram>{{cite journal |url=https://www.osti.gov/servlets/purl/1896856 |title=The Status and Ambitions of the US Heavy Element Program |first1=J. |last1=Gates |first2=J. |last2=Pore |first3=H. |last3=Crawford |first4=D. |last4=Shaughnessy |first5=M. A. |last5=Stoyer |date=25 October 2022 |website=osti.gov |publisher= |access-date=13 November 2022 |doi=10.2172/1896856 |osti=1896856 |s2cid=253391052 |quote=}}</ref> The experiment began at a cyclotron while RIKEN upgraded its linear accelerators; the upgrade was completed in 2020.<ref>{{Cite web|url=https://www.nishina.riken.jp/about/greeting_e.html|title = Greeting &#124; RIKEN Nishina Center|quote=With the completion of the upgrade of the linear accelerator and BigRIPS at the beginning of 2020, the RNC aims to synthesize new elements from element 119 and beyond.|date=1 April 2020|first=Hiroyoshi|last=Sakurai}}</ref> Bombardment may be continued with both machines until the first event is observed; the experiment is currently running intermittently for at least 100 days per year.<ref name="ball19">{{cite journal |last=Ball |first=P. |title=Extreme chemistry: experiments at the edge of the periodic table |date=2019 |journal=Nature |volume=565 |issue=7741 |pages=552–555 |issn=1476-4687 |doi=10.1038/d41586-019-00285-9|pmid=30700884 |bibcode=2019Natur.565..552B |s2cid=59524524 |doi-access=free |url=https://www.nature.com/magazine-assets/d41586-019-00285-9/d41586-019-00285-9.pdf |quote="We started the search for element 119 last June," says RIKEN researcher Hideto En'yo. "It will certainly take a long time — years and years — so we will continue the same experiment intermittently for 100 or more days per year, until we or somebody else discovers it."}}</ref><ref name="sakai" /> The RIKEN team's efforts are being financed by the [[Emperor of Japan]].<ref>{{cite web |url=https://eic.rsc.org/feature/the-hunt-is-on/3008580.article |title=The hunt is on |last1=Chapman |first1=Kit |last2=Turner |first2=Kristy |date=13 February 2018 |website=Education in Chemistry |publisher=Royal Society of Chemistry |access-date=28 June 2019 |quote=The hunt for element 113 was almost abandoned because of lack of resources, but this time Japan’s emperor is bankrolling Riken’s efforts to extend the periodic table to its eighth row.}}</ref> The team at the JINR plans to attempt synthesis of element 119 in the future, probably using the {{sup|243}}Am + {{sup|54}}Cr reaction, but a precise timeframe has not been publicly released.<ref>{{cite web |url=http://www.jinr.ru/posts/jinr-presented-largest-periodic-table-to-dubna/ |title=JINR presented largest Periodic Table to Dubna |author=Joint Institute for Nuclear Research |date=24 July 2021 |website=jinr.ru |publisher=Joint Institute for Nuclear Research |access-date=27 January 2022}}</ref><ref>{{cite web |url=http://www.jinr.ru/posts/superheavy-element-factory-overview-of-obtained-results/ |title=Superheavy Element Factory: overview of obtained results |author= |date=24 August 2023 |website= |publisher=Joint Institute for Nuclear Research |access-date=7 December 2023 |quote=}}</ref>

==== Unbinilium (E120) ====
Following their success in obtaining [[oganesson]] by the reaction between [[californium-249|249Cf]] and [[calcium-48|48Ca]] in 2006, the team at the [[Joint Institute for Nuclear Research]] (JINR) in [[Dubna]] started similar experiments in March–April 2007, in hope of creating [[unbinilium|element 120]] (unbinilium) from nuclei of [[iron-58|58Fe]] and [[plutonium-244|244Pu]].<ref>{{cite news|url=https://www.llnl.gov/str/April07/pdfs/04_07.4.pdf|title=A New Block on the Periodic Table|date=April 2007|publisher=Lawrence Livermore National Laboratory|access-date=2008-01-18|archive-url=https://web.archive.org/web/20080528130457/https://www.llnl.gov/str/April07/pdfs/04_07.4.pdf|archive-date=2008-05-28|url-status=dead}}</ref><ref>{{cite web |url=http://wwwinfo.jinr.ru/plan/ptp-2007/e751004.htm |title=Synthesis of New Nuclei and Study of Nuclear Properties and Heavy-Ion Reaction Mechanisms |last1=Itkis |first1=M. G. |last2=Oganessian |first2=Yu. Ts. |date=2007 |website=jinr.ru |publisher=Joint Institute for Nuclear Research |access-date=23 September 2016}}</ref> Isotopes of unbinilium are predicted to have alpha decay half-lives of the order of [[microsecond]]s.<ref name=prc08ADNDT08>{{cite journal|journal=Physical Review C|volume=77|page=044603|year=2008|title=Search for long lived heaviest nuclei beyond the valley of stability|first1=P. Roy |last1=Chowdhury |first2=C. |last2=Samanta |first3= D. N. |last3=Basu|doi=10.1103/PhysRevC.77.044603|bibcode = 2008PhRvC..77d4603C|issue=4|arxiv = 0802.3837 |s2cid=119207807}}</ref><ref name="sciencedirect1">{{cite journal|journal=[[Atomic Data and Nuclear Data Tables]] |volume=94|pages=781–806|year=2008|title=Nuclear half-lives for α -radioactivity of elements with 100 ≤ Z ≤ 130|author=Chowdhury, R. P.|author2=Samanta, C.|author3=Basu, D.N.|doi=10.1016/j.adt.2008.01.003|bibcode = 2008ADNDT..94..781C|issue=6|arxiv = 0802.4161 |s2cid=96718440}}</ref> Initial analysis revealed that no atoms of element 120 were produced, providing a limit of 400&nbsp;[[barn (unit)|fb]] for the [[cross section (physics)|cross section]] at the energy studied.<ref name=Oganessian120>{{cite journal|journal=Phys. Rev. C|volume=79|page=024603|date=2009|title=Attempt to produce element 120 in the 244Pu+58Fe reaction|doi=10.1103/PhysRevC.79.024603|last1=Oganessian|first1=Yu. Ts.|last2=Utyonkov|first2=V.|last3=Lobanov|first3=Yu.|last4=Abdullin|first4=F.|last5=Polyakov|first5=A.|last6=Sagaidak|first6=R.|last7=Shirokovsky|first7=I.|last8=Tsyganov|first8=Yu.|last9=Voinov|first9=A.|issue=2 |bibcode = 2009PhRvC..79b4603O|display-authors=8 }}</ref>

:{{nuclide|plutonium|244}} + {{nuclide|iron|58}} → 302120* → no atoms

The Russian team planned to upgrade their facilities before attempting the reaction again.<ref name=Oganessian120 />

In April 2007, the team at the [[GSI Helmholtz Centre for Heavy Ion Research]] in [[Darmstadt]], Germany, attempted to create element 120 using [[uranium]]-238 and [[nickel]]-64:<ref name=GSI08>{{cite report|last=Hoffman|first=S.|display-authors=etal|title=Probing shell effects at Z=120 and N=184|date=2008|publisher=GSI Scientific Report|page=131}}</ref>

:{{nuclide|uranium|238}} + {{nuclide|nickel|64}} → 302120* → no atoms

No atoms were detected providing a limit of 1.6&nbsp;[[barn (unit)|pb]] for the cross section at the energy provided. The GSI repeated the experiment with higher sensitivity in three separate runs in April–May 2007, January–March 2008, and September–October 2008, all with negative results, reaching a cross section limit of 90&nbsp;fb.<ref name=GSI08 />

In June–July 2010, and again in 2011, after upgrading their equipment to allow the use of more radioactive targets, scientists at the GSI attempted the more asymmetrical fusion reaction:<ref name=Hofmann2016 />

:{{nuclide|curium|248}} + {{nuclide|chromium|54}} → 302120 → no atoms

It was expected that the change in reaction would quintuple the probability of synthesizing element 120,<ref>{{cite web |url=https://www.gsi.de/de/work/forschung/nustarenna/nustarenna_divisions/she_physik/research/super_heavy_elements/future_projects.htm |title=Searching for the island of stability |author=GSI |date= 2012-04-05|website=www.gsi.de |publisher=GSI |access-date=23 September 2016}}</ref> as the yield of such reactions is strongly dependent on their asymmetry.<ref name=Zagrebaev/> Three correlated signals were observed that matched the predicted alpha decay energies of 299120 and its [[decay product|daughter]] 295Og, as well as the experimentally known decay energy of its granddaughter 291[[livermorium|Lv]]. However, the lifetimes of these possible decays were much longer than expected, and the results could not be confirmed.<ref name=Hoffman>{{cite web |url=https://jphysplus.iop.org/2015/10/02/weighty-matters-sigurd-hofmann-on-the-heaviest-of-nuclei/ |title=Weighty matters: Sigurd Hofmann on the heaviest of nuclei |last1=Adcock |first1=Colin |date=2 October 2015 |website=JPhys+ |access-date=23 September 2016 |archive-date=18 July 2023 |archive-url=https://web.archive.org/web/20230718025533/https://jphysplus.iop.org/2015/10/02/weighty-matters-sigurd-hofmann-on-the-heaviest-of-nuclei/ |url-status=dead }}</ref><ref>{{Citation |last=Hofmann |first=S. |title=Search for isotopes of element 120 on the island of shn |date=2015-05-12 |url=https://www.worldscientific.com/doi/abs/10.1142/9789814699464_0023 |work=Exotic Nuclei |pages=213–224 |publisher=WORLD SCIENTIFIC |doi=10.1142/9789814699464_0023 |bibcode=2015exon.conf..213H |isbn=978-981-4699-45-7 |access-date=2022-02-27}}</ref><ref name=Hofmann2016>{{cite journal |last1=Hofmann |first1=S. |last2=Heinz |first2=S. |first3=R. |last3=Mann |first4=J. |last4=Maurer |first5=G. |last5=Münzenberg |first6=S. |last6=Antalic |first7=W. |last7=Barth |first8=H. G. |last8=Burkhard |first9=L. |last9=Dahl |first10=K. |last10=Eberhardt |first11=R. |last11=Grzywacz |first12=J. H. |last12=Hamilton |first13=R. A. |last13=Henderson |first14=J. M. |last14=Kenneally |first15=B. |last15=Kindler |first16=I. |last16=Kojouharov |first17=R. |last17=Lang |first18=B. |last18=Lommel |first19=K. |last19=Miernik |first20=D. |last20=Miller |first21=K. J. |last21=Moody |first22=K. |last22=Morita |first23=K. |last23=Nishio |first24=A. G. |last24=Popeko |first25=J. B. |last25=Roberto |first26=J. |last26=Runke |first27=K. P. |last27=Rykaczewski |first28=S. |last28=Saro |first29=C. |last29=Scheidenberger |first30=H. J. |last30=Schött |first31=D. A. |last31=Shaughnessy |first32=M. A. |last32=Stoyer |first33=P. |last33=Thörle-Popiesch |first34=K. |last34=Tinschert |first35=N. |last35=Trautmann |first36=J. |last36=Uusitalo |first37=A. V. |last37=Yeremin |date=2016 |title=Review of even element super-heavy nuclei and search for element 120 |journal=The European Physical Journal A |volume=2016 |issue=52 |pages=180 |doi=10.1140/epja/i2016-16180-4|bibcode=2016EPJA...52..180H |s2cid=124362890 |url=https://zenodo.org/record/897926 }}</ref>

In August–October 2011, a different team at the GSI using the TASCA facility tried a new, even more asymmetrical reaction:<ref name=Duellmann>{{cite web |url=http://www.yumpu.com/en/document/view/7293741/superheavy-element-research-superheavy-element-research |title=Superheavy Element Research: News from GSI and Mainz |last1=Düllmann |first1=C. E. |date=20 October 2011 |access-date=23 September 2016}}</ref><ref name=Yakushev />

:{{nuclide|californium|249}} + {{nuclide|titanium|50}} → 299120* → no atoms

This was also tried unsuccessfully the next year during the aforementioned attempt to make element 119 in the 249Bk+50Ti reaction, as 249Bk decays to 249Cf. Because of its asymmetry,<ref>{{cite journal |last1=Siwek-Wilczyńska |first1=K. |last2=Cap |first2=T. |last3=Wilczyński |first3=J. |date=April 2010 |title=How can one synthesize the element ''Z'' = 120? |journal=International Journal of Modern Physics E |volume=19 |issue=4 |pages=500 |doi=10.1142/S021830131001490X|bibcode=2010IJMPE..19..500S }}</ref> the reaction between 249Cf and 50Ti was predicted to be the most favorable practical reaction for synthesizing unbinilium, although it is also somewhat cold. No unbinilium atoms were identified, implying a limiting cross-section of 200&nbsp;fb.<ref name=Yakushev>{{cite web |url=http://asrc.jaea.go.jp/soshiki/gr/chiba_gr/workshop3/&Yakushev.pdf |title=Superheavy Element Research at TASCA |last1=Yakushev |first1=A. |date=2012 |website=asrc.jaea.go.jp |access-date=23 September 2016}}</ref> Jens Volker Kratz predicted the actual maximum cross-section for producing element 120 by any of these reactions to be around 0.1&nbsp;fb;<ref name=Kratz/> in comparison, the world record for the smallest cross section of a successful reaction was 30&nbsp;fb for the reaction 209Bi(70Zn,n)278[[nihonium|Nh]],<ref name=Zagrebaev/> and Kratz predicted a maximum cross-section of 20&nbsp;fb for producing the neighbouring element 119.<ref name=Kratz/> If these predictions are accurate, then synthesizing element 119 would be at the limits of current technology, and synthesizing element 120 would require new methods.<ref name=Kratz/>

In May 2021, the JINR announced plans to investigate the 249Cf+50Ti reaction in their new facility. However, the 249Cf target would have had to be made by the [[Oak Ridge National Laboratory]] in the United States,<ref>{{cite web |url=http://www.jinr.ru/posts/how-are-new-chemical-elements-born/ |title=How are new chemical elements born? |last1=Sokolova |first1=Svetlana |last2=Popeko |first2=Andrei |date=24 May 2021 |website=jinr.ru |publisher=JINR |access-date=4 November 2021 |quote=Previously, we worked mainly with calcium. This is element 20 in the Periodic Table. It was used to bombard the target. And the heaviest element that can be used to make a target is californium, 98. Accordingly, 98 + 20 is 118. That is, to get element 120, we need to proceed to the next particle. This is most likely titanium: 22 + 98 = 120. There is still much work to adjust the system. I don’t want to get ahead of myself, but if we can successfully conduct all the model experiments, then the first experiments on the synthesis of element 120 will probably start this year.}}</ref> and after the [[Russian invasion of Ukraine]] began in February 2022, collaboration between the JINR and other institutes completely ceased due to sanctions.<ref name=ft>{{cite news |last=Ahuja |first=Anjana |date=18 October 2023 |title=Even the periodic table must bow to the reality of war |url=https://www.ft.com/content/6b6b0afc-39b2-4955-af5a-d0ea6b4d8306 |work=Financial Times |location= |access-date=20 October 2023}}</ref> Consequently, the JINR now plans to try the 248Cm+54Cr reaction instead. A preparatory experiment for the use of 54Cr projectiles was conducted in late 2023, successfully synthesising 288Lv in the 238U+54Cr reaction,<ref name=Lv288>{{cite news |url=http://www.jinr.ru/posts/v-lyar-oiyai-vpervye-v-mire-sintezirovan-livermorij-288/ |title=В ЛЯР ОИЯИ впервые в мире синтезирован ливерморий-288 |trans-title=Livermorium-288 was synthesized for the first time in the world at FLNR JINR |language=ru |date=23 October 2023 |publisher=Joint Institute for Nuclear Research |access-date=18 November 2023}}</ref> and the hope is for experiments to synthesise element 120 to begin by 2025.<ref>{{cite news |last=Mayer |first=Anastasiya |date=31 May 2023 |language=ru |title="Большинство наших партнеров гораздо мудрее политиков" |trans-title=Most of our partners are much wiser than politicians |url=https://www.vedomosti.ru/technology/characters/2023/05/31/977789-bolshinstvo-nashih-partnerov-mudree-politikov |work=[[Vedomosti]] |location= |access-date=15 August 2023 |quote=В этом году мы фактически завершаем подготовительную серию экспериментов по отладке всех режимов ускорителя и масс-спектрометров для синтеза 120-го элемента. Научились получать высокие интенсивности ускоренного хрома и титана. Научились детектировать сверхтяжелые одиночные атомы в реакциях с минимальным сечением. Теперь ждем, когда закончится наработка материала для мишени на реакторах и сепараторах у наших партнеров в «Росатоме» и в США: кюрий, берклий, калифорний. Надеюсь, что в 2025 г. мы полноценно приступим к синтезу 120-го элемента.}}</ref>

Starting from 2022,<ref name=usprogram/> plans have also been made to use 88-inch cyclotron in the [[Lawrence Berkeley National Laboratory]] (LBNL) in [[Berkeley, California|Berkeley]], [[California]], United States to attempt to make new elements using 50Ti projectiles. The plan is to first test them on a plutonium target to create [[livermorium]] (element 116) in late 2023. If that is successful, an attempt to make element 120 in the 249Cf+50Ti reaction will begin, probably in 2024 at the earliest.<ref>{{cite news |last=Chapman |first=Kit |date=10 October 2023 |title=Berkeley Lab to lead US hunt for element 120 after breakdown of collaboration with Russia |url=https://www.chemistryworld.com/news/berkeley-lab-to-lead-us-hunt-for-element-120-after-breakdown-of-collaboration-with-russia/4018207.article |work=Chemistry World |location= |access-date=20 October 2023}}</ref><ref>{{cite web |url=https://physicalsciences.lbl.gov/2023/10/16/berkeley-lab-to-test-new-approach-to-making-superheavy-elements/ |title=Berkeley Lab to Test New Approach to Making Superheavy Elements |last=Biron |first=Lauren |date=16 October 2023 |website=lbl.gov |publisher=[[Lawrence Berkeley National Laboratory]] |access-date=20 October 2023 |quote=}}</ref>

==== Unbiunium (E121) ====
The synthesis of [[unbiunium|element 121]] (unbiunium) was first attempted in 1977 by bombarding a target of [[uranium-238]] with [[copper]]-65 ions at the [[Gesellschaft für Schwerionenforschung]] in [[Darmstadt]], Germany:
:{{nuclide|uranium|238}} + {{nuclide|copper|65}} → 303121* → no atoms
No atoms were identified.<ref name=beyonduranium>{{cite book |last=Hofmann |first=Sigurd |date=2002 |title=On Beyond Uranium |publisher=Taylor & Francis |page=[https://archive.org/details/onbeyonduraniumj0000hofm/page/105 105] |isbn=978-0-415-28496-7 |url=https://archive.org/details/onbeyonduraniumj0000hofm/page/105 }}</ref>

==== Unbibium (E122) ====
The first attempts to synthesize [[unbibium|element 122]] (unbibium) were performed in 1972 by [[Georgy Flerov|Flerov]] et al. at the [[Joint Institute for Nuclear Research]] (JINR), using the heavy-ion induced hot fusion reactions:<ref name="emsley"/>

:{{nuclide|uranium|238}} + {{nuclide|zinc|66,68}} → 304, 306122* → no atoms

These experiments were motivated by early predictions on the existence of an [[island of stability]] at ''N''&nbsp;=&nbsp;184 and ''Z''&nbsp;>&nbsp;120. No atoms were detected and a yield limit of 5&nbsp;[[Barn (unit)|nb]] (5,000&nbsp;[[barn (unit)|pb]]) was measured. Current results (see [[flerovium]]) have shown that the sensitivity of these experiments were too low by at least 3 orders of magnitude.<ref name=superlourds>{{cite journal|last1=Epherre|first1=M.|last2=Stephan|first2=C.|date=1975|title=Les éléments superlourds|language=fr|journal=Le Journal de Physique Colloques|volume=11|issue=36|pages=C5–159–164|url=https://core.ac.uk/download/pdf/46775464.pdf|doi=10.1051/jphyscol:1975541}}</ref>

In 2000, the [[Gesellschaft für Schwerionenforschung]] (GSI) Helmholtz Center for Heavy Ion Research performed a very similar experiment with much higher sensitivity:<ref name="emsley">{{cite book|last=Emsley|first=John|title=Nature's Building Blocks: An A-Z Guide to the Elements|edition=New|year=2011|publisher=Oxford University Press|location=New York, NY|isbn=978-0-19-960563-7|page=588}}</ref>

:{{nuclide|uranium|238}} + {{nuclide|zinc|70}} → 308122* → no atoms

These results indicate that the synthesis of such heavier elements remains a significant challenge and further improvements of beam intensity and experimental efficiency is required. The sensitivity should be increased to 1&nbsp;[[barn (unit)|fb]] in the future for more quality results.

Another unsuccessful attempt to synthesize element 122 was carried out in 1978 at the GSI Helmholtz Center, where a natural [[erbium]] target was bombarded with [[xenon-136]] ions:<ref name="emsley"/>

:{{nuclide|erbium|''nat''}} + {{nuclide|xenon|136}} → 298, 300, 302, 303, 304, 306122* → no atoms

In particular, the reaction between 170Er and 136Xe was expected to yield alpha-emitters with half-lives of microseconds that would decay down to isotopes of [[flerovium]] with half-lives perhaps increasing up to several hours, as flerovium is predicted to lie near the center of the [[island of stability]]. After twelve hours of irradiation, nothing was found in this reaction. Following a similar unsuccessful attempt to synthesize element 121 from 238U and 65Cu, it was concluded that half-lives of superheavy nuclei must be less than one microsecond or the cross sections are very small.<ref name=EndPT>{{cite book|last=Hofmann|first=Sigurd|title=On Beyond Uranium: Journey to the End of the Periodic Table|year=2014|publisher=CRC Press|isbn=978-0415284950|page=[https://archive.org/details/onbeyonduraniumj0000hofm/page/105 105]|url=https://archive.org/details/onbeyonduraniumj0000hofm/page/105}}</ref> More recent research into synthesis of superheavy elements suggests that both conclusions are true.<ref name=Zagrebaev /><ref name=Karpov>{{cite web |url=http://cyclotron.tamu.edu/she2015/assets/pdfs/presentations/Karpov_SHE_2015_TAMU.pdf |title=Superheavy Nuclei: which regions of nuclear map are accessible in the nearest studies |last1=Karpov |first1=A |last2=Zagrebaev |first2=V |last3=Greiner |first3=W |date=2015 |website=cyclotron.tamu.edu |publisher=Texas A & M University |access-date=30 October 2018}}</ref> The two attempts in the 1970s to synthesize element 122 were both propelled by the research investigating whether superheavy elements could potentially be naturally occurring.<ref name="emsley"/>

Several experiments studying the fission characteristics of various superheavy compound nuclei such as 306122* were performed between 2000 and 2004 at the [[Flerov Laboratory of Nuclear Reactions]]. Two nuclear reactions were used, namely 248Cm + 58Fe and 242Pu + 64Ni.<ref name="emsley"/> The results reveal how superheavy nuclei fission predominantly by expelling [[nuclear shell model|closed shell]] nuclei such as 132Sn (''Z''&nbsp;=&nbsp;50, ''N''&nbsp;=&nbsp;82). It was also found that the yield for the fusion-fission pathway was similar between 48Ca and 58Fe projectiles, suggesting a possible future use of 58Fe projectiles in superheavy element formation.<ref name="www1.jinr.ru">see Flerov lab annual reports 2000–2004 inclusive http://www1.jinr.ru/Reports/Reports_eng_arh.html</ref>

==== Unbiquadium (E124) ====
{{Further|Unbiquadium}}
Scientists at [[GANIL]] (Grand Accélérateur National d'Ions Lourds) attempted to measure the direct and delayed fission of compound nuclei of elements with ''Z'' = 114, 120, and 124 in order to probe [[nuclear shell|shell]] effects in this region and to pinpoint the next spherical proton shell. This is because having complete nuclear shells (or, equivalently, having a [[magic number (physics)|magic number]] of [[proton]]s or [[neutron]]s) would confer more stability on the nuclei of such superheavy elements, thus moving closer to the [[island of stability]]. In 2006, with full results published in 2008, the team provided results from a reaction involving the bombardment of a natural [[germanium]] target with uranium ions:

:{{nuclide|uranium|238}} + {{nuclide|germanium|''nat''}} → 308, 310, 311, 312, 314124* → ''fission''

The team reported that they had been able to identify compound nuclei fissioning with half-lives > 10−18 s. This result suggests a strong stabilizing effect at ''Z'' = 124 and points to the next proton shell at ''Z'' > 120, not at ''Z'' = 114 as previously thought. A compound nucleus is a loose combination of [[nucleon]]s that have not arranged themselves into nuclear shells yet. It has no internal structure and is held together only by the collision forces between the target and projectile nuclei. It is estimated that it requires around 10−14&nbsp;s for the nucleons to arrange themselves into nuclear shells, at which point the compound nucleus becomes a [[nuclide]], and this number is used by [[IUPAC]] as the minimum [[half-life]] a claimed isotope must have to potentially be recognised as being discovered. Thus, the GANIL experiments do not count as a discovery of [[element 124]].<ref name="emsley"/>

The fission of the compound nucleus 312124 was also studied in 2006 at the tandem ALPI heavy-ion accelerator at the [[Laboratori Nazionali di Legnaro]] (Legnaro National Laboratories) in Italy:<ref name="thomas">{{cite journal|last1=Thomas|first1=R.G.|last2=Saxena|first2=A.|last3=Sahu|first3=P.K. |last4=Choudhury|first4=R.K.|last5=Govil|first5=I.M.|last6=Kailas|first6=S. |last7=Kapoor|first7=S.S.|last8=Barubi|first8=M.|last9=Cinausero|first9=M. |last10=Prete|first10=G.|last11=Rizzi|first11=V.|last12=Fabris|first12=D. |last13=Lunardon|first13=M.|last14=Moretto|first14=S.|last15=Viesti|first15=G. |last16=Nebbia|first16=G.|last17=Pesente|first17=S.|last18=Dalena|first18=B. |last19=D'Erasmo|first19=G.|last20=Fiore|first20=E.M.|last21=Palomba|first21=M. |last22=Pantaleo|first22=A.|last23=Paticchio|first23=V.|last24=Simonetti|first24=G. |last25=Gelli|first25=N.|last26=Lucarelli|first26=F.|date=2007|title=Fission and binary fragmentation reactions in 80Se+208Pb and 80Se+232Th systems|journal=Physical Review C|volume=75|issue=2|pages=024604–1–024604–9|doi=10.1103/PhysRevC.75.024604|hdl=2158/776924|hdl-access=free}}</ref>

:{{nuclide|thorium|232}} + {{nuclide|selenium|80}} → 312124* → ''fission''

Similarly to previous experiments conducted at the JINR ([[Joint Institute for Nuclear Research]]), [[fission product|fission fragments]] clustered around [[doubly magic]] nuclei such as 132Sn (''Z'' = 50, ''N'' = 82), revealing a tendency for superheavy nuclei to expel such doubly magic nuclei in fission.<ref name="www1.jinr.ru"/> The average number of neutrons per fission from the 312124 compound nucleus (relative to lighter systems) was also found to increase, confirming that the trend of heavier nuclei emitting more neutrons during fission continues into the superheavy mass region.<ref name=thomas />

==== Unbipentium (E125) ====
The first and only attempt to synthesize element 125 (unbipentium) was conducted in Dubna in 1970{{endash}}1971 using [[zinc]] ions and an [[americium-243]] target:<ref name=superlourds />

:{{nuclide|americium|243}} + {{nuclide|zinc|66, 68}} → 309, 311125* → no atoms

No atoms were detected, and a cross section limit of 5 nb was determined. This experiment was motivated by the possibility of greater stability for nuclei around ''Z''&nbsp;~&nbsp;126 and ''N''&nbsp;~&nbsp;184,<ref name=superlourds /> though more recent research suggests the island of stability may instead lie at a lower atomic number (such as [[copernicium]], ''Z'' = 112), and the synthesis of heavier elements such as element 125 will require more sensitive experiments.<ref name=Zagrebaev />

==== Unbihexium (E126) ====
{{Further|Unbihexium}}
The first and only attempt to synthesize [[unbihexium|element 126]] (unbihexium), which was unsuccessful, was performed in 1971 at [[CERN]] (European Organization for Nuclear Research) by René Bimbot and John M. Alexander using the hot fusion reaction:<ref name="emsley"/>

:{{nuclide|thorium|232}} + {{nuclide|krypton|84}} → 316126* → no atoms

[[decay energy|High-energy]] (13–15&nbsp;[[electronvolt|MeV]]) [[alpha particles]] were observed and taken as possible evidence for the synthesis of element 126. Subsequent unsuccessful experiments with higher sensitivity suggest that the 10&nbsp;[[barn (unit)|mb]] sensitivity of this experiment was too low; hence, the formation of element 126 nuclei in this reaction is highly unlikely.<ref name=Transuraniumppl>{{cite book|last1=Hoffman|first1=D.C |last2=Ghiorso|first2=A.|last3=Seaborg|first3=G.T.|title=The Transuranium People: The Inside Story |publisher=Imperial College Press|date=2000|isbn=978-1-86094-087-3}}</ref>

==== Unbiseptium (E127) ====
The first and only attempt to synthesize element 127 (unbiseptium), which was unsuccessful, was performed in 1978 at the [[UNILAC]] accelerator at the GSI Helmholtz Center, where a natural [[tantalum]] target was bombarded with [[xenon]]-136 ions:<ref name="emsley"/>

:{{nuclide|tantalum|''nat''}} + {{nuclide|xenon|136}} → 316, 317127* → no atoms

===Searches in nature===
A study in 1976 by a group of American researchers from several universities proposed that [[primordial element|primordial]] superheavy elements, mainly [[livermorium]], elements 124, 126, and 127, could be a cause of unexplained radiation damage (particularly [[radiohalos]]) in minerals.<ref name=Transuraniumppl /> This prompted many researchers to search for them in nature from 1976 to 1983. A group led by Tom Cahill, a professor at the [[University of California, Davis|University of California at Davis]], claimed in 1976 that they had detected [[alpha particle]]s and [[X-rays]] with the right energies to cause the damage observed, supporting the presence of these elements. In particular, the presence of long-lived (on the order of 109 years) nuclei of elements 124 and 126, along with their decay products, at an abundance of 10−11 relative to their possible [[congener (chemistry)|congener]]s [[uranium]] and [[plutonium]], was conjectured.<ref name=symposium>{{cite book |editor1-last=Lodhi |editor1-first=M.A.K. |title=Superheavy Elements: Proceedings of the International Symposium on Superheavy Elements |location= Lubbock, Texas |publisher=Pergamon Press |date=March 1978 |isbn=978-0-08-022946-1}}</ref> Others claimed that none had been detected, and questioned the proposed characteristics of primordial superheavy nuclei.<ref name=Transuraniumppl /> In particular, they cited that any such superheavy nuclei must have a closed neutron shell at ''N''&nbsp;=&nbsp;184 or ''N''&nbsp;=&nbsp;228, and this necessary condition for enhanced stability only exists in neutron deficient isotopes of livermorium or neutron rich isotopes of the other elements that would not be [[beta-decay stable isobars|beta-stable]]<ref name=Transuraniumppl /> unlike most naturally occurring isotopes.<ref name=nubase>{{cite journal|last1=Audi|first1=G.|last2=Kondev|first2=F.G.|last3=Wang|first3=M.|last4=Huang|first4=W.J.| last5=Naimi|first5=S.|title=The NUBASE2016 evaluation of nuclear properties|url=http://amdc.in2p3.fr/nubase/2017Audi03.pdf|journal=Chinese Physics C|volume=41|issue=3|date=2017|pages=030001|doi=10.1088/1674-1137/41/3/030001|bibcode=2017ChPhC..41c0001A}}</ref> This activity was also proposed to be caused by nuclear transmutations in natural [[cerium]], raising further ambiguity upon this claimed observation of superheavy elements.<ref name=Transuraniumppl />

On April 24, 2008, a group led by [[Amnon Marinov]] at the [[Hebrew University of Jerusalem]] claimed to have found single atoms of 292122 in naturally occurring [[thorium]] deposits at an abundance of between 10−11 and 10−12 relative to thorium.<ref name=arxiv/> The claim of Marinov et al. was criticized by a part of the scientific community. Marinov claimed that he had submitted the article to the journals ''[[Nature (journal)|Nature]]'' and ''[[Nature Physics]]'' but both turned it down without sending it for peer review.<ref>[[Royal Society of Chemistry]], "[http://rsc.org/chemistryworld/News/2008/May/02050802.asp Heaviest element claim criticised] {{Webarchive|url=https://web.archive.org/web/20160304042449/http://rsc.org/chemistryworld/News/2008/May/02050802.asp |date=2016-03-04 }}", Chemical World.</ref> The 292122 atoms were claimed to be [[superdeformation|superdeformed]] or [[hyperdeformation|hyperdeformed]] [[nuclear isomer|isomers]], with a half-life of at least 100 million years.<ref name="emsley"/>

A criticism of the technique, previously used in purportedly identifying lighter [[thorium]] isotopes by [[mass spectrometry]],<ref name="thorium">{{cite journal |journal=Phys. Rev. C |title=Existence of long-lived isomeric states in naturally-occurring neutron-deficient Th isotopes |year=2007 |volume=76 |page=021303(R) |doi=10.1103/PhysRevC.76.021303 |first1=A. |last1=Marinov |first2=I. |last2=Rodushkin |first3=Y. |last3=Kashiv |first4=L. |last4=Halicz |first5=I. |last5=Segal |first6=A. |last6=Pape |first7=R. V. |last7=Gentry |first8=H. W. |last8=Miller |first9= D. |last9=Kolb |first10=R. |last10=Brandt |arxiv = nucl-ex/0605008 |bibcode = 2007PhRvC..76b1303M |issue=2 |s2cid=119443571 }}</ref> was published in ''[[Physical Review C]]'' in 2008.<ref>{{cite journal |journal=Phys. Rev. C |title=Comment on 'Existence of long-lived isomeric states in naturally-occurring neutron-deficient Th isotopes' |year=2009 |volume=79 |pages=049801 |doi=10.1103/PhysRevC.79.049801 |author1=R. C. Barber |author2=J. R. De Laeter |bibcode = 2009PhRvC..79d9801B |issue=4 }}</ref> A rebuttal by the Marinov group was published in ''Physical Review C'' after the published comment.<ref>{{cite journal |journal=Phys. Rev. C |title=Reply to "Comment on 'Existence of long-lived isomeric states in naturally-occurring neutron-deficient Th isotopes'" |year=2009 |volume=79 |pages=049802 |doi=10.1103/PhysRevC.79.049802 |author1=A. Marinov |author2=I. Rodushkin |author3=Y. Kashiv |author4=L. Halicz |author5=I. Segal |author6=A. Pape |author7=R. V. Gentry |author8=H. W. Miller |author9=D. Kolb |author10=R. Brandt |bibcode = 2009PhRvC..79d9802M |issue=4 }}</ref>

A repeat of the thorium-experiment using the superior method of [[Accelerator mass spectrometry|Accelerator Mass Spectrometry]] (AMS) failed to confirm the results, despite a 100-fold better sensitivity.<ref>{{cite journal |journal=Phys. Rev. C |title=Search for long-lived isomeric states in neutron-deficient thorium isotopes |year=2008 |volume=78 |page= 064313 |doi=10.1103/PhysRevC.78.064313 |author1=J. Lachner |author2=I. Dillmann |author3=T. Faestermann |author4=G. Korschinek |author5=M. Poutivtsev |author6=G. Rugel |bibcode = 2008PhRvC..78f4313L |issue=6 |arxiv = 0907.0126 |s2cid=118655846 }}</ref> This result throws considerable doubt on the results of the Marinov collaboration with regard to their claims of long-lived isotopes of [[thorium]],<ref name="thorium"/> [[roentgenium]]<ref name="roentgenium">{{cite journal |last1=Marinov |first1=A. |last2=Rodushkin |first2=I. |last3=Pape |first3=A. |last4=Kashiv |first4=Y. |last5=Kolb |first5=D. |last6=Brandt |first6=R. |last7=Gentry |first7=R. V. |last8=Miller |first8=H. W. |last9=Halicz |first9=L. |first10=I. |last10=Segal |year=2009 |title=Existence of Long-Lived Isotopes of a Superheavy Element in Natural Au |journal=[[International Journal of Modern Physics E]] |volume=18 |number=3 |pages=621–629 |doi=10.1142/S021830130901280X |url=http://www.phys.huji.ac.il/~marinov/publications/Au_paper_IJMPE_73.pdf |access-date=February 12, 2012 |arxiv=nucl-ex/0702051 |bibcode=2009IJMPE..18..621M |s2cid=119103410 |url-status=dead |archiveurl=https://web.archive.org/web/20140714210340/http://www.phys.huji.ac.il/~marinov/publications/Au_paper_IJMPE_73.pdf |archive-date=July 14, 2014 }}</ref> and element 122.<ref name=arxiv>{{cite journal |last=Marinov |first=A. |author2=Rodushkin, I. |author3=Kolb, D. |author4=Pape, A. |author5=Kashiv, Y. |author6=Brandt, R. |author7=Gentry, R. V. |author8= Miller, H. W. |title=Evidence for a long-lived superheavy nucleus with atomic mass number A=292 and atomic number Z=~122 in natural Th |journal= International Journal of Modern Physics E|year=2010 |arxiv=0804.3869 |bibcode = 2010IJMPE..19..131M |doi = 10.1142/S0218301310014662 |volume=19 |issue=1 |pages=131–140 |s2cid=117956340 }}</ref> It is still possible that traces of unbibium might only exist in some thorium samples, although this is unlikely.<ref name="emsley"/>

The possible extent of primordial superheavy elements on Earth today is uncertain. Even if they are confirmed to have caused the radiation damage long ago, they might now have decayed to mere traces, or even be completely gone.<ref name="emsley2">{{cite book|last=Emsley|first=John|title=Nature's Building Blocks: An A–Z Guide to the Elements |edition=New |year=2011 |publisher=Oxford University Press|location=New York |isbn=978-0-19-960563-7|page=592}}</ref> It is also uncertain if such superheavy nuclei may be produced naturally at all, as [[spontaneous fission]] is expected to terminate the [[r-process]] responsible for heavy element formation between mass number 270 and 290, well before elements beyond 120 may be formed.<ref>{{cite journal|last1=Petermann |first1=I|last2=Langanke|first2=K.|last3=Martínez-Pinedo|first3=G.|last4=Panov|first4=I.V |last5=Reinhard|first5=P.G.|last6=Thielemann|first6=F.K.|date=2012|title=Have superheavy elements been produced in nature?|journal=European Physical Journal A|volume=48|issue=122|page=122|url=https://www.researchgate.net/publication/229156774|doi=10.1140/epja/i2012-12122-6|arxiv=1207.3432|bibcode=2012EPJA...48..122P|s2cid=119264543}}</ref>

A recent hypothesis tries to explain the spectrum of [[Przybylski's Star]] by naturally occurring [[flerovium]] and element 120.<ref name=Isotope1>{{cite web|url=https://sites.psu.edu/astrowright/2017/03/16/przybylskis-star-iii-neutron-stars-unbinilium-and-aliens/|title=Przybylski's Star III: Neutron Stars, Unbinilium, and aliens|author=Jason Wright|date=16 March 2017|access-date=31 July 2018}}</ref><ref name=Isotope2>{{Cite journal|title=Isotope shift and search for metastable superheavy elements in astrophysical data|journal = Physical Review A|volume = 95|issue = 6|pages = 062515|author1=V. A. Dzuba|author2=V. V. Flambaum|author3=J. K. Webb|arxiv=1703.04250|doi = 10.1103/PhysRevA.95.062515|year = 2017|bibcode=2017PhRvA..95f2515D|s2cid = 118956691}}</ref><ref name=SciShowSpace>Archived at [https://ghostarchive.org/varchive/youtube/20211211/XKD0pFYewu4 Ghostarchive]{{cbignore}} and the [https://web.archive.org/web/20190605060157/https://www.youtube.com/watch?v=XKD0pFYewu4 Wayback Machine]{{cbignore}}: {{cite web|url=https://www.youtube.com/watch?v=XKD0pFYewu4|title=This Star Might Be Hiding Undiscovered Elements. Przybylski's Star|author=SciShow Space|website=youtube.com|date=31 July 2018|access-date=31 July 2018}}{{cbignore}}</ref>

==Predicted properties of eighth-period elements==
Element 118, [[oganesson]], is the heaviest element that has been synthesized. The next two elements, [[ununennium|elements 119]] and [[unbinilium|120]], should form an 8s series and be an [[alkali metal|alkali]] and [[alkaline earth metal]] respectively. Beyond element 120, the [[superactinide]] series is expected to begin, when the 8s electrons and the filling of the 8p1/2, 7d3/2, 6f, and 5g subshells determine the chemistry of these elements. Complete and accurate [[Coupled cluster#Types of coupled-cluster methods|CCSD]] calculations are not available for elements beyond 122 because of the extreme complexity of the situation: the 5g, 6f, and 7d orbitals should have about the same energy level, and in the region of element 160, the 9s, 8p3/2, and 9p1/2 orbitals should also be about equal in energy. This will cause the electron shells to mix so that the [[block (periodic table)|block]] concept no longer applies very well, and will also result in novel chemical properties that will make positioning some of these elements in a periodic table very difficult.<ref name=Haire/>

[[File:Energy eigenvalues superheavy.svg|thumb|center|640px|Energy eigenvalues (in eV) for the outermost electrons of elements with Z = 100 through 172, predicted using Dirac–Fock calculations. The − and + signs refer to orbitals with decreased or increased azimuthal quantum number from spin–orbit splitting respectively: p− is p1/2, p+ is p3/2, d− is d3/2, d+ is d5/2, f− is f5/2, f+ is f7/2, g− is g7/2, and g+ is g9/2.<ref name=BFricke/>]]

===Chemical and physical properties===

====Elements 119 and 120====
{{main|Ununennium|Unbinilium}}
<div style="float: right; margin: 1px; font-size:85%;">
:{| class="wikitable"
|+ Some predicted properties of elements 119 and 120<ref name="Fricke"/><ref name=Haire/>
! Property
! 119
! 120
|-
! [[Standard atomic weight]]
| [322]
| [325]
|-
! [[Periodic table group|Group]]
| [[alkali metal|1]]
| [[alkaline earth metal|2]]
|-
! Valence [[electron configuration]]
| 8s1
| 8s2
|-
! Stable [[oxidation state]]s
| '''1''', 3
| '''2''', 4
|-
! First [[ionization energy]]
| 463.1 [[kilojoule per mole|kJ/mol]]
| 563.3 kJ/mol
|-
! [[Metallic radius]]
| 260 pm
| 200 pm
|-
! [[Density]]
| 3 g/cm3
| 7 g/cm3
|-
! [[Melting point]]
| {{convert|0–30|C|F|sigfig=2}}
| {{convert|680|C|F|sigfig=2}}
|-sigfig=
! [[Boiling point]]
| {{convert|630|C|F|sigfig=2}}
| {{convert|1700|C|F|sigfig=2}}
|}
</div>
The first two elements of period&nbsp;8 will be ununennium and unbinilium, elements 119 and 120. Their [[electron configuration]]s should have the 8s orbital being filled. This orbital is relativistically stabilized and contracted; thus, elements&nbsp;119 and 120 should be more like [[rubidium]] and [[strontium]] than their immediate neighbours above, [[francium]] and [[radium]]. Another effect of the relativistic contraction of the 8s orbital is that the [[atomic radius|atomic radii]] of these two elements should be about the same as those of francium and radium. They should behave like normal [[alkali metal|alkali]] and [[alkaline earth metal]]s (albeit less reactive than their immediate vertical neighbours), normally forming +1 and +2 [[oxidation state]]s respectively, but the relativistic destabilization of the 7p3/2 subshell and the relatively low [[ionization energy|ionization energies]] of the 7p3/2 electrons should make higher oxidation states like +3 and +4 (respectively) possible as well.<ref name="Fricke"/><ref name=Haire>{{cite book| title=The Chemistry of the Actinide and Transactinide Elements| editor1-last=Morss|editor2-first=Norman M.| editor2-last=Edelstein| editor3-last=Fuger|editor3-first=Jean| last1=Hoffman|first1=Darleane C. |last2=Lee |first2=Diana M. |last3=Pershina |first3=Valeria |chapter=Transactinides and the future elements| publisher= [[Springer Science+Business Media]]| year=2006| isbn=978-1-4020-3555-5| location=Dordrecht, The Netherlands| edition=3rd| ref=CITEREFHaire2006}}</ref>

====Superactinides====
The superactinides may be considered to range from elements 121 through 157, which can be classified as the 5g and 6f elements of the eighth period, together with the first 7d element.<ref name=nefedov/> In the superactinide series, the 7d3/2, 8p1/2, 6f5/2 and 5g7/2 shells should all fill simultaneously.<ref name="BFricke"/> This creates very complicated situations, so much so that complete and accurate CCSD calculations have been done only for elements 121 and 122.<ref name=Haire/> The first superactinide, [[unbiunium]] (element 121), should be similar to [[lanthanum]] and [[actinium]]:<ref>{{Cite journal | last1 = Waber | first1 = J. T. | title = SCF Dirac–Slater Calculations of the Translawrencium Elements | doi = 10.1063/1.1672054 | journal = The Journal of Chemical Physics | volume = 51 | issue = 2 | page = 664| year = 1969 |bibcode = 1969JChPh..51..664W }}</ref> its main oxidation state should be +3, although the closeness of the valence subshells' energy levels may permit higher oxidation states, just as in elements 119 and 120.<ref name=Haire/> Relativistic stabilization of the 8p subshell should result in a ground-state 8s28p1 valence electron configuration for element 121, in contrast to the ds2 configurations of lanthanum and actinium;<ref name=Haire/> nevertheless, this anomalous configuration does not appear to affect its calculated chemistry, which remains similar to that of actinium.<ref name=Amador>{{cite journal |last1=Amador |first1=Davi H. T. |last2=de Oliveira |first2=Heibbe C. B. |first3=Julio R. |last3=Sambrano |first4=Ricardo |last4=Gargano |first5=Luiz Guilherme M. |last5=de Macedo |date=12 September 2016 |title=4-Component correlated all-electron study on Eka-actinium Fluoride (E121F) including Gaunt interaction: Accurate analytical form, bonding and influence on rovibrational spectra |journal=Chemical Physics Letters |volume=662 |pages=169–175 |doi=10.1016/j.cplett.2016.09.025|bibcode=2016CPL...662..169A |hdl=11449/168956 |hdl-access=free }}</ref> Its first [[ionization energy]] is predicted to be 429.4&nbsp;kJ/mol, which would be lower than those of all known elements except for the [[alkali metals]] [[potassium]], [[rubidium]], [[caesium]], and [[francium]]: this value is even lower than that of the period 8 alkali metal ununennium (463.1&nbsp;kJ/mol). Similarly, the next superactinide, [[unbibium]] (element 122), may be similar to [[cerium]] and [[thorium]], with a main oxidation state of +4, but would have a ground-state 7d18s28p1 or 8s28p2 valence electron configuration,<ref name="Umemoto"/> unlike thorium's 6d27s2 configuration. Hence, its first [[ionization energy]] would be smaller than thorium's (Th: 6.3&nbsp;[[electronvolt|eV]]; element 122: 5.6&nbsp;eV) because of the greater ease of ionizing unbibium's 8p1/2 electron than thorium's 6d electron.<ref name=Haire/> The collapse of the 5g orbital itself is delayed until around element 125; the electron configurations of the 119-electron isoelectronic series are expected to be [Og]8s1 for elements 119 through 122, [Og]6f1 for elements 123 and 124, and [Og]5g1 for element 125 onwards.<ref name=5gchem/>

In the first few superactinides, the binding energies of the added electrons are predicted to be small enough that they can lose all their valence electrons; for example, [[unbihexium]] (element 126) could easily form a +8 oxidation state, and even higher oxidation states for the next few elements may be possible. Element 126 is also predicted to display a variety of other [[oxidation state]]s: recent calculations have suggested a stable [[Fluoride|monofluoride]] 126F may be possible, resulting from a bonding interaction between the 5g&nbsp;[[Atomic orbital|orbital]] on element 126 and the 2[[p-orbital|p]]&nbsp;orbital on [[fluorine]].<ref name=Jacoby>{{Cite journal|last=Jacoby|first=Mitch|title=As-yet-unsynthesized superheavy atom should form a stable diatomic molecule with fluorine|journal=Chemical & Engineering News|year=2006|volume=84|issue=10|pages=19|doi=10.1021/cen-v084n010.p019a}}</ref> Other predicted oxidation states include +2, +4, and +6; +4 is expected to be the most usual oxidation state of unbihexium.<ref name="BFricke"/> The superactinides from unbipentium (element 125) to unbiennium (element 129) are predicted to exhibit a +6 oxidation state and form [[hexafluorides]], though 125F6 and 126F6 are predicted to be relatively weakly bound.<ref name="5gchem">{{cite journal|last1=Dongon|first1=J.P.|last2=Pyykkö|first2=P.|date=2017|title=Chemistry of the 5g elements. Relativistic calculations on hexafluorides|journal= Angewandte Chemie International Edition|volume=56|issue=34|pages=10132–10134|doi=10.1002/anie.201701609|pmid=28444891|s2cid=205400592 |url=https://hal-cea.archives-ouvertes.fr/cea-01515489/document}}</ref> The [[bond dissociation energy|bond dissociation energies]] are expected to greatly increase at element 127 and even more so at element 129. This suggests a shift from strong ionic character in fluorides of element 125 to more covalent character, involving the 8p orbital, in fluorides of element 129. The bonding in these superactinide hexafluorides is mostly between the highest 8p subshell of the superactinide and the 2p subshell of fluorine, unlike how uranium uses its 5f and 6d orbitals for bonding in [[uranium hexafluoride]].<ref name=5gchem />

Despite the ability of early superactinides to reach high oxidation states, it has been calculated that the 5g electrons will be most difficult to ionize; the 1256+ and 1267+ ions are expected to bear a 5g1 configuration, similar to the 5f1 configuration of the Np6+ ion.<ref name="PT172"/><ref name=5gchem /> Similar behavior is observed in the low chemical activity of the 4f electrons in [[lanthanide]]s; this is a consequence of the 5g orbitals being small and deeply buried in the electron cloud.<ref name="PT172"/> The presence of electrons in g-orbitals, which do not exist in the ground state electron configuration of any currently known element, should allow presently unknown [[orbital hybridization|hybrid]] orbitals to form and influence the chemistry of the superactinides in new ways, although the absence of ''g'' electrons in known elements makes predicting superactinide chemistry more difficult.<ref name="Fricke"/>
<div style="margin:0 auto; font-size:85%;">
:{| class="wikitable"
|+ Some predicted compounds of the superactinides (X = a [[halogen]])<ref name="PT172"/><ref name=5gchem /><ref>{{cite journal |last=Makhyoun |first=M. A. |date=October 1988 |title=On the electronic structure of 5g1 complexes of element 125: a quasi-relativistic MS-Xα study |journal=Journal de Chimie Physique et de Physico-Chimie Biologique |volume=85 |issue=10 |pages=917–24 |doi=10.1051/jcp/1988850917 |bibcode=1988JCP....85..917M }}</ref>
!
! 121
! 122
! 123
! 124
! 125
! 126
! 127
! 128
! 129
! 132
! 142
! 143
! 144
! 145
! 146
! 148
! 153
! 154
! 155
! 156
! 157
|-
! Compound
| 121X3
| 122X4
| 123X5
| 124X6
| 125F 125F6 {{chem|125O|2|2+}}
| 126F 126F6 126O4
| 127F6
| 128F6
| 129F 129F6
|
| 142X4 142X6
| 143F6
| 144X6 {{chem|144O|2|2+}} 144F8 144O4
| 145F6
|
| 148O6
|
|
|
|
|
|-
! Analogs
| [[lanthanum|La]]X3 [[actinium|Ac]]X3
| [[cerium|Ce]]X4 [[thorium|Th]]X4
|
|
| {{chem|[[neptunium|Np]]O|2|2+}}
|
|
|
|
|
| [[thorium tetrafluoride|ThF4]]
|
| [[uranium hexafluoride|UF6]] [[uranyl|{{chem|UO|2|2+}}]] [[plutonium|Pu]]F8 PuO4
|
|
| [[uranium hexoxide|UO6]]
|
|
|
|
|
|-
! Oxidation states
| 3
| 4
| 5
| 6
| 1, 6, 7
| 1, 2, 4, 6, 8
| 6
| 6
| 1, 6
| 6
| 4, 6
| 6, 8
| 3, 4, 5, 6, 8
| 6
| 8
| 12
| 3
| 0, 2
| 3, 5
| 2
| 3
|}
</div>{{clear}}
In the later superactinides, the oxidation states should become lower. By element 132, the predominant most stable oxidation state will be only +6; this is further reduced to +3 and +4 by element 144, and at the end of the superactinide series it will be only +2 (and possibly even 0) because the 6f shell, which is being filled at that point, is deep inside the electron cloud and the 8s and 8p1/2 electrons are bound too strongly to be chemically active. The 5g shell should be filled at element 144 and the 6f shell at around element 154, and at this region of the superactinides the 8p1/2 electrons are bound so strongly that they are no longer active chemically, so that only a few electrons can participate in chemical reactions. Calculations by Fricke et al. predict that at element 154, the 6f shell is full and there are no d- or other electron [[wave function]]s outside the chemically inactive 8s and 8p1/2 shells. This may cause element 154 to be rather [[reactivity (chemistry)|unreactive]] with [[noble gas]]-like properties.<ref name="Fricke"/><ref name=Haire/> Calculations by Pyykkö nonetheless expect that at element 155, the 6f shell is still chemically ionisable: 1553+ should have a full 6f shell, and the fourth ionisation potential should be between those of [[terbium]] and [[dysprosium]], both of which are known in the +4 state.<ref name=PT172/>

Similarly to the [[lanthanide contraction|lanthanide and actinide contractions]], there should be a superactinide contraction in the superactinide series where the [[ionic radius|ionic radii]] of the superactinides are smaller than expected. In the [[lanthanide]]s, the contraction is about 4.4&nbsp;pm per element; in the [[actinide]]s, it is about 3&nbsp;pm per element. The contraction is larger in the lanthanides than in the actinides due to the greater localization of the 4f wave function as compared to the 5f wave function. Comparisons with the wave functions of the outer electrons of the lanthanides, actinides, and superactinides lead to a prediction of a contraction of about 2&nbsp;pm per element in the superactinides; although this is smaller than the contractions in the lanthanides and actinides, its total effect is larger due to the fact that 32 electrons are filled in the deeply buried 5g and 6f shells, instead of just 14 electrons being filled in the 4f and 5f shells in the lanthanides and actinides respectively.<ref name="Fricke"/>

[[Pekka Pyykkö]] divides these superactinides into three series: a 5g series (elements 121 to 138), an 8p1/2 series (elements 139 to 140), and a 6f series (elements 141 to 155), also noting that there would be a great deal of overlapping between energy levels and that the 6f, 7d, or 8p1/2 orbitals could well also be occupied in the early superactinide atoms or ions. He also expects that they would behave more like "superlanthanides", in the sense that the 5g electrons would mostly be chemically inactive, similarly to how only one or two 4f electrons in each lanthanide are ever ionized in chemical compounds. He also predicted that the possible oxidation states of the superactinides might rise very high in the 6f series, to values such as +12 in element 148.<ref name="PT172"/>

Andrey Kulsha has called the thirty-six elements 121 to 156 "ultransition" elements and has proposed to split them into two series of eighteen each, one from elements 121 to 138 and another from elements 139 to 156. The first would be analogous to the lanthanides, with oxidation states mainly ranging from +4 to +6, as the filling of the 5g shell dominates and neighbouring elements are very similar to each other, creating an analogy to [[uranium]], [[neptunium]], and [[plutonium]]. The second would be analogous to the actinides: at the beginning (around elements in the 140s) very high oxidation states would be expected as the 6f shell rises above the 7d one, but after that the typical oxidation states would lower and in elements in the 150s onwards the 8p1/2 electrons would stop being chemically active. Because the two rows are separated by the addition of a complete 5g18 subshell, they could be considered analogues of each other as well.<ref name=primefan/><ref name=sicius/>

As an example from the late superactinides, element 156 is expected to exhibit mainly the +2 oxidation state, on account of its electron configuration with easily removed 7d2 electrons over a stable [Og]5g186f148s28p{{su|p=2|b=1/2}} core. It can thus be considered a heavier congener of [[nobelium]], which likewise has a pair of easily removed 7s2 electrons over a stable [Rn]5f14 core, and is usually in the +2 state (strong oxidisers are required to obtain nobelium in the +3 state).<ref name=primefan/> Its first ionization energy should be about 400&nbsp;kJ/mol and its metallic radius approximately 170&nbsp;picometers. With a relative atomic mass of around 445&nbsp;u,<ref name=Fricke/> it should be a very heavy metal with a density of around 26&nbsp;g/cm3.

====Elements 157 to 166====
The 7d transition metals in period 8 are expected to be elements 157 to 166. Although the 8s and 8p1/2 electrons are bound so strongly in these elements that they should not be able to take part in any chemical reactions, the 9s and 9p1/2 levels are expected to be readily available for hybridization.<ref name="Fricke"/><ref name=Haire/> These 7d elements should be similar to the 4d elements [[yttrium]] through [[cadmium]].<ref name=primefan/> In particular, element 164 with a 7d109s0 electron configuration shows clear analogies with [[palladium]] with its 4d105s0 electron configuration.<ref name=BFricke/>

The noble metals of this series of transition metals are not expected to be as noble as their lighter homologues, due to the absence of an outer ''s'' shell for shielding and also because the 7d shell is strongly split into two subshells due to relativistic effects. This causes the first ionization energies of the 7d transition metals to be smaller than those of their lighter congeners.<ref name="Fricke"/><ref name=Haire/><ref name="BFricke"/>

Theoretical interest in the chemistry of unhexquadium is largely motivated by theoretical predictions that it, especially the isotopes 472164 and 482164 (with 164 [[proton]]s and 308 or 318 [[neutron]]s), would be at the center of a hypothetical second [[island of stability]] (the first being centered on [[copernicium]], particularly the isotopes 291Cn, 293Cn, and 296Cn which are expected to have half-lives of centuries or millennia).<ref name=magickoura /><ref name="Kratz">
{{cite conference
|last1=Kratz |first1=J. V.
|date=5 September 2011
|title=The Impact of Superheavy Elements on the Chemical and Physical Sciences
|url=http://tan11.jinr.ru/pdf/06_Sep/S_1/02_Kratz.pdf
|conference=4th International Conference on the Chemistry and Physics of the Transactinide Elements
|access-date=27 August 2013
}}</ref><ref name="eurekalert.org">{{cite web|url=http://www.eurekalert.org/pub_releases/2008-04/acs-nse031108.php|title=Nuclear scientists eye future landfall on a second 'island of stability'|date=6 April 2008|website=EurekAlert!|access-date=2015-12-17}}</ref><ref name="link.springer.com">{{cite journal | doi = 10.1007/BF01406719 | volume = 228 | issue = 5 | title = Investigation of the stability of superheavy nuclei aroundZ=114 andZ=164 | journal = Zeitschrift für Physik | pages = 371–386 | bibcode = 1969ZPhy..228..371G | year = 1969 | last1 = Grumann | first1 = Jens | last2 = Mosel | first2 = Ulrich | last3 = Fink | first3 = Bernd | last4 = Greiner | first4 = Walter | s2cid = 120251297 }}</ref>

Calculations predict that the 7d electrons of element 164 (unhexquadium) should participate very readily in chemical reactions, so that it should be able to show stable +6 and +4 oxidation states in addition to the normal +2 state in [[aqueous solution]]s with strong [[ligand]]s. Element 164 should thus be able to form compounds like 164([[carbonyl|CO]])4, 164([[phosphorus trifluoride|PF3]])4 (both [[tetrahedral molecular geometry|tetrahedral]] like the corresponding palladium compounds), and {{chem|164([[cyanide|CN]])|2|2-}} ([[linear molecular geometry|linear]]), which is very different behavior from that of [[lead]], which element 164 would be a heavier [[Homologous series|homologue]] of if not for relativistic effects. Nevertheless, the divalent state would be the main one in aqueous solution (although the +4 and +6 states would be possible with stronger ligands), and unhexquadium(II) should behave more similarly to lead than unhexquadium(IV) and unhexquadium(VI).<ref name=Haire/><ref name="BFricke">{{Cite journal |last1=Fricke |first1=Burkhard |year=1975 |title=Superheavy elements: a prediction of their chemical and physical properties |journal=Recent Impact of Physics on Inorganic Chemistry |volume=21 |pages=[https://archive.org/details/recentimpactofph0000unse/page/89 89–144] |doi=10.1007/BFb0116498 |url=https://archive.org/details/recentimpactofph0000unse/page/89 |access-date=4 October 2013 |series=Structure and Bonding |isbn=978-3-540-07109-9 }}</ref>

Element 164 is expected to be a soft [[Lewis acid]] and have Ahrlands softness parameter close to 4&nbsp;[[electronvolt|eV]]. It should be at most moderately reactive, having a first ionization energy that should be around 685&nbsp;kJ/mol, comparable to that of [[molybdenum]].<ref name="Fricke"/><ref name="BFricke"/> Due to the [[lanthanide contraction|lanthanide, actinide, and superactinide contractions]], element 164 should have a metallic radius of only 158&nbsp;[[picometer|pm]], very close to that of the much lighter [[magnesium]], despite its expected atomic weight of around 474&nbsp;[[atomic mass unit|u]] which is about 19.5&nbsp;times the atomic weight of magnesium.<ref name="Fricke"/> This small radius and high weight cause it to be expected to have an extremely high density of around 46&nbsp;g·cm−3, over twice that of [[osmium]], currently the most dense element known, at 22.61&nbsp;g·cm−3; element 164 should be the second most dense element in the first 172 elements in the periodic table, with only its neighbor unhextrium (element 163) being more dense (at 47&nbsp;g·cm−3).<ref name="Fricke"/> Metallic element 164 should have a very large cohesive energy ([[enthalpy]] of crystallization) due to its [[Covalent bond|covalent]] bonds, most probably resulting in a high melting point. In the metallic state, element 164 should be quite noble and analogous to palladium and [[platinum]]. Fricke et al. suggested some formal similarities to [[oganesson]], as both elements have closed-shell configurations and similar ionisation energies, although they note that while oganesson would be a very bad noble gas, element 164 would be a good noble metal.<ref name="BFricke"/>

Elements 165 (unhexpentium) and 166 (unhexhexium), the last two 7d metals, should behave similarly to [[alkali metal|alkali]] and [[alkaline earth metal]]s when in the +1 and +2 oxidation states respectively. The 9s electrons should have ionization energies comparable to those of the 3s electrons of [[sodium]] and [[magnesium]], due to relativistic effects causing the 9s electrons to be much more strongly bound than non-relativistic calculations would predict. Elements 165 and 166 should normally exhibit the +1 and +2 oxidation states respectively, although the ionization energies of the 7d electrons are low enough to allow higher oxidation states like +3 for element 165. The oxidation state +4 for element 166 is less likely, creating a situation similar to the lighter elements in groups 11 and 12 (particularly [[gold]] and [[mercury (element)|mercury]]).<ref name="Fricke"/><ref name=Haire/> As with mercury but not copernicium, ionization of element 166 to 1662+ is expected to result in a 7d10 configuration corresponding to the loss of the s-electrons but not the d-electrons, making it more analogous to the lighter "less relativistic" group 12 elements zinc, cadmium, and mercury.<ref name=PT172/>

<div style="float: center; margin: 1px; font-size:85%;">
:{| class="wikitable"
|+ Some predicted properties of elements 156–166 The metallic radii and densities are first approximations.<ref name="Fricke"/><ref name="PT172"/><ref name=Haire/> Most analogous group is given first, followed by other similar groups.<ref name="BFricke"/>
! Property
! 156
! 157
! 158
! 159
! 160
! 161
! 162
! 163
! 164
! 165
! 166
|-
! [[Standard atomic weight]]
| [445]
| [448]
| [452]
| [456]
| [459]
| [463]
| [466]
| [470]
| [474]
| [477]
| [481]
|-
! [[Periodic table group|Group]]
| [[ytterbium|Yb]] group
| [[group 3 element|3]]
| [[group 4 element|4]]
| [[group 5 element|5]]
| [[group 6 element|6]]
| [[group 7 element|7]]
| [[group 8 element|8]]
| [[group 9 element|9]]
| [[group 10 element|10]]
| [[group 11 element|11]] (1)
| [[group 12 element|12]] (2)
|-
! Valence [[electron configuration]]
| 7d2
| 7d3
| 7d4
| 7d5
| 7d6
| 7d7
| 7d8
| 7d9
| 7d10
| 7d10 9s1
| 7d10 9s2
|-
! Stable [[oxidation state]]s
| '''2'''
| '''3'''
| '''4'''
| '''1''', '''5'''
| '''2''', '''6'''
| '''3''', '''7'''
| '''4''', '''8'''
| '''5'''
| '''0''', '''2''', '''4''', '''6'''
| '''1''', '''3'''
| '''2'''
|-
! First [[ionization energy]]
| 400 kJ/mol
| 450 kJ/mol
| 520 kJ/mol
| 340 kJ/mol
| 420 kJ/mol
| 470 kJ/mol
| 560 kJ/mol
| 620 kJ/mol
| 690 kJ/mol
| 520 kJ/mol
| 630 kJ/mol
|-
! [[Metallic radius]]
| 170 pm
| 163 pm
| 157 pm
| 152 pm
| 148 pm
| 148 pm
| 149 pm
| 152 pm
| 158 pm
| 250 pm
| 200 pm
|-
! [[Density]]
| 26 g/cm3
| 28 g/cm3
| 30 g/cm3
| 33 g/cm3
| 36 g/cm3
| 40 g/cm3
| 45 g/cm3
| 47 g/cm3
| 46 g/cm3
| 7 g/cm3
| 11 g/cm3
|}
</div>

====Elements 167 to 172====
The next six elements on the periodic table are expected to be the last main-group elements in their period,<ref name="PT172"/> and are likely to be similar to the 5p elements [[indium]] through [[xenon]].<ref name=primefan/> In elements 167 to 172, the 9p1/2 and 8p3/2 shells will be filled. Their energy [[eigenvalue]]s are so close together that they behave as one combined p-subshell, similar to the non-relativistic 2p and 3p subshells. Thus, the [[inert-pair effect]] does not occur and the most common oxidation states of elements 167 to 170 are expected to be +3, +4, +5, and +6 respectively. Element 171 (unseptunium) is expected to show some similarities to the [[halogen]]s, showing various oxidation states ranging from −1 to +7, although its physical properties are expected to be closer to that of a metal. Its electron affinity is expected to be 3.0&nbsp;[[electronvolt|eV]], allowing it to form H171, analogous to a [[hydrogen halide]]. The 171− ion is expected to be a [[HSAB|soft base]], comparable to [[iodide]] (I−). Element 172 (unseptbium) is expected to be a [[noble gas]] with chemical behaviour similar to that of xenon, as their ionization energies should be very similar (Xe, 1170.4&nbsp;kJ/mol; element 172, 1090&nbsp;kJ/mol). The only main difference between them is that element 172, unlike xenon, is expected to be a [[liquid]] or a [[solid]] at [[standard temperature and pressure]] due to its much higher atomic weight.<ref name="Fricke"/> Unseptbium is expected to be a strong [[Lewis acid]], forming fluorides and oxides, similarly to its lighter congener xenon.<ref name="BFricke"/>

Because of some analogy of elements 165–172 to periods 2 and 3, Fricke et al. considered them to form a ninth period of the periodic table, while the eighth period was taken by them to end at the noble metal element 164. This ninth period would be similar to the second and third period in having no transition metals.<ref name="BFricke"/> That being said, the analogy is incomplete for elements 165 and 166; although they do start a new s-shell (9s), this is above a d-shell, making them chemically more similar to groups 11 and 12.<ref name=actrev/>

<div style="float: center; margin: 1px; font-size:85%;">
:{| class="wikitable"
|+ Some predicted properties of elements 167–172 The metallic or covalent radii and densities are first approximations.<ref name="Fricke"/><ref name=Haire/><ref name="BFricke"/>
! Property
! 167
! 168
! 169
! 170
! 171
! 172
|-
! [[Standard atomic weight]]
| [485]
| [489]
| [493]
| [496]
| [500]
| [504]
|-
! [[Periodic table group|Group]]
| [[boron group|13]]
| [[carbon group|14]]
| [[pnictogen|15]]
| [[chalcogen|16]]
| [[halogen|17]]
| [[noble gas|18]]
|-
! Valence [[electron configuration]]
| 9s2 9p1
| 9s2 9p2
| 9s2 9p2 8p1
| 9s2 9p2 8p2
| 9s2 9p2 8p3
| 9s2 9p2 8p4
|-
! Stable [[oxidation state]]s
| '''3'''
| '''4'''
| '''5'''
| '''6'''
| '''−1''', '''3''', '''7'''
| '''0''', '''4''', '''6''', '''8'''
|-
! First [[ionization energy]]
| 620 kJ/mol
| 720 kJ/mol
| 800 kJ/mol
| 890 kJ/mol
| 984 kJ/mol
| 1090 kJ/mol
|-
! [[Metallic radius|Metallic]] or [[covalent radius]]
| 190 pm
| 180 pm
| 175 pm
| 170 pm
| 165 pm
| 220 pm
|-
! [[Density]]
| 17 g/cm3
| 19 g/cm3
| 18 g/cm3
| 17 g/cm3
| 16 g/cm3
| 9 g/cm3
|}
</div>

====Beyond element 172====
Beyond element 172, there is the potential to fill the 6g, 7f, 8d, 10s, 10p1/2, and perhaps 6h11/2 shells. These electrons would be very loosely bound, potentially rendering extremely high oxidation states reachable, though the electrons would become more tightly bound as the ionic charge rises. Thus, there will probably be another very long transition series, like the superactinides.<ref name="BFricke"/>

In element 173 (unsepttrium), the outermost electron might enter the 6g7/2, 9p3/2, or 10s subshells. Because spin–orbit interactions would create a very large energy gap between these and the 8p3/2 subshell, this outermost electron is expected to be very loosely bound and very easily lost to form a 173+ cation. As a result, element 173 is expected to behave chemically like an alkali metal, and one that might be far more reactive than even [[caesium]] (francium and element 119 being less reactive than caesium due to relativistic effects):<ref name="BFricke1977">{{cite journal |last1=Fricke |first1=Burkhard |year=1977 |title=Dirac–Fock–Slater calculations for the elements Z = 100, fermium, to Z = 173 |journal=Recent Impact of Physics on Inorganic Chemistry |volume=19 |pages=83–192 |doi=10.1016/0092-640X(77)90010-9 |url=http://kobra.bibliothek.uni-kassel.de/bitstream/urn:nbn:de:hebis:34-2008071622807/1/Fricke_Dirac_1977.pdf |access-date=25 February 2016|bibcode = 1977ADNDT..19...83F }}</ref><ref name=primefan>{{cite book |editor-last=Kolevich |editor-first=T. A. |last1=Kulsha |first1=Andrey |chapter=Есть ли граница у таблицы Менделеева? |trans-chapter=Is there a boundary to the Mendeleev table? |date=2011 |title=Удивительный мир веществ и их превращений |trans-title=The wonderful world of substances and their transformations |url=http://www.primefan.ru/stuff/chem/ptable/ptable.pdf |location=Minsk |publisher=Национальный институт образования (National Institute of Education) |pages=5–19 |isbn=978-985-465-920-6 |language=ru |access-date=8 September 2018}}</ref> the calculated ionisation energy for element 173 is 3.070&nbsp;eV,<ref name=eliav2023/> compared to the experimentally known 3.894&nbsp;eV for caesium. Element 174 (unseptquadium) may add an 8d electron and form a closed-shell 1742+ cation; its calculated ionisation energy is 3.614&nbsp;eV.<ref name=eliav2023/>

Element 184 (unoctquadium) was significantly targeted in early predictions, as it was originally speculated that 184 would be a proton magic number: it is predicted to have an electron configuration of [172] 6g5 7f4 8d3, with at least the 7f and 8d electrons chemically active. Its chemical behaviour is expected to be similar to [[uranium]] and [[neptunium]], as further ionisation past the +6 state (corresponding to removal of the 6g electrons) is likely to be unprofitable; the +4 state should be most common in aqueous solution, with +5 and +6 reachable in solid compounds.<ref name="Fricke"/><ref name="BFricke"/><ref name=Penneman>{{cite journal |last1=Penneman |first1=R. A. |last2=Mann |first2=J. B. |last3=Jørgensen |first3=C. K. |date=February 1971 |title=Speculations on the chemistry of superheavy elements such as Z = 164 |journal=Chemical Physics Letters |volume=8 |issue=4 |pages=321–326 |doi=10.1016/0009-2614(71)80054-4 |bibcode=1971CPL.....8..321P }}</ref>

===End of the periodic table===
The number of physically possible elements is unknown. A low estimate is that the periodic table may end soon after the [[island of stability]],<ref name=EB>{{cite encyclopedia|last1=Seaborg|first1=Glenn T.|url=https://www.britannica.com/EBchecked/topic/603220/transuranium-element|title=transuranium element (chemical element)|encyclopedia=Encyclopædia Britannica|date=c. 2006|access-date=2010-03-16}}</ref> which is expected to center on ''Z''&nbsp;=&nbsp;126, as the extension of the periodic and [[nuclide]] tables is restricted by the proton and the neutron [[Nuclear drip line|drip lines]] and stability toward alpha decay and spontaneous fission.<ref>{{cite journal | first1=S. |last1=Cwiok|first2=P.-H.|last2=Heenen |first3=W.|last3=Nazarewicz |year=2005|title=Shape coexistence and triaxiality in the superheavy nuclei|journal=Nature|volume=433|bibcode = 2005Natur.433..705C |doi = 10.1038/nature03336 | issue=7027 | pmid=15716943 | pages=705–9|s2cid=4368001}}</ref> One calculation by Y. Gambhir ''et al.'', analyzing [[nuclear binding energy]] and stability in various decay channels, suggests a limit to the existence of bound nuclei at ''Z''&nbsp;=&nbsp;146.<ref name=limit146>{{cite journal|last1=Gambhir|first1=Y. K.|last2=Bhagwat|first2=A.|last3=Gupta|first3=M.|title=The highest limiting Z in the extended periodic table|date=2015|journal=Journal of Physics G: Nuclear and Particle Physics|volume=42|issue=12|pages=125105|doi=10.1088/0954-3899/42/12/125105|url= https://www.researchgate.net/publication/284213926|bibcode=2015JPhG...42l5105G}}</ref> Other predictions of an end to the periodic table include ''Z''&nbsp;=&nbsp;128 ([[John Emsley]]) and ''Z''&nbsp;=&nbsp;155 (Albert Khazan).<ref name="emsley"/>

====Elements above the atomic number 137====
It is a "folk legend" among physicists that [[Richard Feynman]] suggested that neutral atoms could not exist for atomic numbers greater than ''Z''&nbsp;=&nbsp;137, on the grounds that the [[Theory of relativity|relativistic]] [[Dirac equation]] predicts that the ground-state energy of the innermost electron in such an atom would be an [[imaginary number]]. Here, the number 137 arises as the inverse of the [[fine-structure constant]]. By this argument, neutral atoms cannot exist beyond atomic number 137, and therefore a periodic table of elements based on electron orbitals breaks down at this point. However, this argument presumes that the atomic nucleus is pointlike. A more accurate calculation must take into account the small, but nonzero, size of the nucleus, which is predicted to push the limit further to ''Z''&nbsp;≈&nbsp;173.<ref name="rsc">{{cite web |url=https://www.chemistryworld.com/opinion/column-the-crucible/3005076.article |title=Would element 137 really spell the end of the periodic table? Philip Ball examines the evidence|author=Philip Ball |date=November 2010 |website=[[Chemistry World]]|publisher=[[Royal Society of Chemistry]] |access-date=2012-09-30}}</ref>

=====Bohr model=====
The [[Bohr model]] exhibits difficulty for atoms with atomic number greater than 137, for the speed of an electron in a [[Atomic orbital|1s electron orbital]], ''v'', is given by

:<math>v = Z \alpha c \approx \frac{Z c}{137.04}</math>

where ''Z'' is the [[atomic number]], and ''α'' is the [[fine-structure constant]], a measure of the strength of electromagnetic interactions.<ref>{{cite book|first1=R. |last1=Eisberg|first2= R.|last2= Resnick|year=1985|title=Quantum Physics of Atoms, Molecules, Solids, Nuclei and Particles|url=https://archive.org/details/quantumphysicsof00eisb |url-access=registration |publisher=[[John Wiley & Sons|Wiley]]|isbn=9780471873730}}</ref> Under this approximation, any element with an atomic number of greater than 137 would require 1s electrons to be traveling faster than ''c'', the [[speed of light]]. Hence, the non-relativistic Bohr model is inaccurate when applied to such an element.

=====Relativistic Dirac equation=====
[[File:1s negative continuum.svg|thumb|right|540px|Energy eigenvalues for the 1s, 2s, 2p1/2 and 2p3/2 shells from solutions of the [[Dirac equation]] (taking into account the finite size of the nucleus) for ''Z''&nbsp;=&nbsp;135–175 (–·–), for the Thomas-Fermi potential (—) and for ''Z''&nbsp;=&nbsp;160–170 with the self-consistent potential (---).<ref name=Fricke/>]]
The [[Theory of relativity|relativistic]] [[Dirac equation]] gives the ground state energy as

:<math>E=\frac{m c^2}{\sqrt{1+\dfrac{Z^2 \alpha^2}{\bigg({n-\left(j+\frac12\right)+\sqrt{\left(j+\frac12\right)^2-Z^ 2\alpha^2}\bigg)}^2}}},</math>

where ''m'' is the rest mass of the electron.<ref>{{cite web |title=Solution of the Dirac Equation for Hydrogen |url=https://quantummechanics.ucsd.edu/ph130a/130_notes/node501.html}}</ref> For ''Z''&nbsp;>&nbsp;137, the wave function of the Dirac ground state is oscillatory, rather than bound, and there is no gap between the positive and negative energy spectra, as in the [[Klein paradox]].<ref>{{cite book|first1=J. D.|last1= Bjorken|first2=S. D.|last2= Drell|year=1964|title=Relativistic Quantum Mechanics|url=https://archive.org/details/relativisticquan0000bjor|url-access=registration|publisher=[[McGraw-Hill]]}}</ref> More accurate calculations taking into account the effects of the finite size of the nucleus indicate that the binding energy first exceeds 2''mc''2 for ''Z''&nbsp;>&nbsp;''Z''cr probably between 168 and 172.<ref name=gamowstates/> For ''Z''&nbsp;>&nbsp;''Z''cr, if the innermost orbital (1s) is not filled, the electric field of the nucleus will [[pair production|pull an electron out of the vacuum]], resulting in the spontaneous emission of a [[positron]].<ref>{{cite journal|first1=W. |last1=Greiner|first2= S. |last2=Schramm |year=2008|title=Resource Letter QEDV-1: The QED vacuum |journal=[[American Journal of Physics]] |volume=76 |issue=6|pages=509 |doi=10.1119/1.2820395|bibcode=2008AmJPh..76..509G}}, and references therein</ref><ref>{{cite journal|last1=Wang|first1=Yang|last2=Wong|first2=Dillon|last3=Shytov|first3=Andrey V.|last4=Brar|first4=Victor W.|last5=Choi|first5=Sangkook|last6=Wu|first6=Qiong|last7=Tsai|first7=Hsin-Zon|last8=Regan|first8=William|last9=Zettl|first9=Alex|author9-link=Alex Zettl|last10=Kawakami|first10=Roland K.|last11=Louie|first11=Steven G.|last12=Levitov|first12=Leonid S.|last13=Crommie|first13=Michael F.|title=Observing Atomic Collapse Resonances in Artificial Nuclei on Graphene|journal=Science|date=May 10, 2013|volume=340|issue=6133|pages=734–737|doi=10.1126/science.1234320|arxiv = 1510.02890 |bibcode = 2013Sci...340..734W|pmid=23470728|s2cid=29384402}}</ref> This diving of the 1s subshell into the negative continuum has often been taken to constitute an "end" to the periodic table,<ref name=PT172/><ref name="rsc"/><ref>{{Cite journal|last1=Indelicato|first1=Paul|last2=Bieroń|first2=Jacek|last3=Jönsson|first3=Per|date=2011-06-01|title=Are MCDF calculations 101% correct in the super-heavy elements range?|url=https://dspace.mah.se/handle/2043/12984|journal=Theoretical Chemistry Accounts|language=en|volume=129|issue=3–5|pages=495–505|doi=10.1007/s00214-010-0887-3|issn=1432-881X|hdl=2043/12984|s2cid=54680128|hdl-access=free}}</ref> but in fact it does not impose such a limit, as such resonances can be interpreted as Gamow states. The accurate description of such states in a multi-electron system, needed to extend calculations and the periodic table past ''Z''cr&nbsp;≈&nbsp;172, are however still open problems.<ref name=gamowstates>{{cite journal |last1=Smits |first1=O. R. |last2=Indelicato |first2=P. |first3=W. |last3=Nazarewicz |first4=M. |last4=Piibeleht |first5=P. |last5=Schwerdtfeger |date=2023 |title=Pushing the limits of the periodic table—A review on atomic relativistic electronic structure theory and calculations for the superheavy elements |url= |journal=Physics Reports |volume=1035 |issue= |pages=1–57 |doi=10.1016/j.physrep.2023.09.004 |access-date=|arxiv=2301.02553 |bibcode=2023PhR..1035....1S }}</ref>

Atoms with atomic numbers above ''Z''cr&nbsp;≈&nbsp;172 have been termed ''supercritical'' atoms. Supercritical atoms cannot be totally ionised because their 1s subshell would be filled by spontaneous pair creation in which an electron-positron pair is created from the negative continuum, with the electron being bound and the positron escaping. However, the strong field around the atomic nucleus is restricted to a very small region of space, so that the [[Pauli exclusion principle]] forbids further spontaneous pair creation once the subshells that have dived into the negative continuum are filled. Elements 173–184 have been termed ''weakly supercritical'' atoms as for them only the 1s shell has dived into the negative continuum; the 2p1/2 shell is expected to join around element 185 and the 2s shell around element 245. Experiments have so far not succeeded in detecting spontaneous pair creation from assembling supercritical charges through the collision of heavy nuclei (e.g. colliding lead with uranium to momentarily give an effective ''Z'' of 174; uranium with uranium gives effective ''Z''&nbsp;=&nbsp;184 and uranium with californium gives effective ''Z''&nbsp;=&nbsp;190).<ref>{{cite book|last1=Reinhardt|first1=Joachim|title = Nuclear Physics: Present and Future|pages=195–210|last2=Greiner|first2=Walter|doi=10.1007/978-3-319-10199-6_19|date=2015|chapter=Probing Supercritical Fields with Real and with Artificial Nuclei|isbn=978-3-319-10198-9}}</ref>

Even though passing ''Z''cr does not mean elements can no longer exist, the increasing concentration of the 1s density close to the nucleus would likely make these electrons more vulnerable to [[electron capture|''K'' electron capture]] as ''Z''cr is approached. For such heavy elements, these 1s electrons would likely spend a significant fraction of time so close to the nucleus that they are actually inside it. This may pose another limit to the periodic table.<ref name=colloq>{{cite journal |title=Colloquium: Superheavy elements: Oganesson and beyond |first1=S. A. |last1=Giuliani |first2=Z. |last2=Matheson |first3=W. |last3=Nazarewicz |first4=E. |last4=Olsen |first5=P.-G. |last5=Reinhard |first6=J. |last6=Sadhukhan |first7=B. |last7=Schtruempf |first8=N. |last8=Schunck |first9=P. |last9=Schwerdtfeger |date=2019 |journal=Reviews of Modern Physics |volume=91 |issue=1 |pages=011001-1–011001-25 |doi=10.1103/RevModPhys.91.011001|bibcode=2019RvMP...91a1001G |s2cid=126906074 |doi-access=free }}</ref>

Because of the factor of ''m'', [[muonic atom]]s become supercritical at a much larger atomic number of around 2200, as [[muon]]s are about 207 times as heavy as electrons.<ref name=gamowstates/>

=====Quark matter=====
{{main|Continent of stability|QCD matter}}
It has also been posited that in the region beyond ''A''&nbsp;>&nbsp;300, an entire "[[continent of stability]]" consisting of a hypothetical phase of stable [[quark matter]], comprising freely flowing [[up quark|up]] and [[down quark|down]] quarks rather than [[quark]]s bound into protons and neutrons, may exist. Such a form of matter is theorized to be a ground state of [[baryonic matter]] with a greater binding energy per [[baryon]] than [[nuclear matter]], favoring the decay of nuclear matter beyond this mass threshold into quark matter. If this state of matter exists, it could possibly be synthesized in the same fusion reactions leading to normal superheavy nuclei, and would be stabilized against fission as a consequence of its stronger binding that is enough to overcome Coulomb repulsion.<ref name="udQM">{{cite journal |last1=Holdom |first1=B. |last2=Ren |first2=J. |last3=Zhang |first3=C. |title=Quark matter may not be strange |date=2018 |journal=Physical Review Letters |volume=120 |issue=1 |pages=222001-1–222001-6 |doi=10.1103/PhysRevLett.120.222001|pmid=29906186 |arxiv=1707.06610 |bibcode=2018PhRvL.120v2001H |s2cid=49216916 }}</ref>

Calculations published in 2020<ref name=udQMnew>{{cite journal |last1=Cheng-Jun |first1=Xia |last2=She-Sheng |first2=Xue |last3=Ren-Xin |first3=Xu |last4=Shan-Gui |first4=Zhou |title=Supercritically charged objects and electron-positron pair creation |doi=10.1103/PhysRevD.101.103031 |journal=Physical Review D |year=2020 |volume=101 |issue=10 |pages=103031|arxiv=2001.03531 |bibcode=2020PhRvD.101j3031X |s2cid=210157134 }}</ref> suggest stability of up-down quark matter (udQM) nuggets against conventional nuclei beyond ''A''&nbsp;~&nbsp;266, and also show that udQM nuggets become supercritical earlier (''Z''cr&nbsp;~&nbsp;163, ''A''&nbsp;~&nbsp;609) than conventional nuclei (''Z''cr&nbsp;~&nbsp;177, ''A''&nbsp;~&nbsp;480).

===Nuclear properties===
{{multiple image
| direction =vertical
| width = 540
| image1 = Island of Stability derived from Zagrebaev.svg
| image2 = Superheavy decay modes predicted.png
| footer = Predicted half-lives (top) and decay modes (bottom) of superheavy nuclei. The line of synthesized proton-rich nuclei is expected to be broken soon after ''Z'' = 120, because of half-lives shorter than 1 microsecond from ''Z'' = [[unbiunium|121]], the increasing contribution of spontaneous fission instead of alpha decay from ''Z'' = [[unbibium|122]] onward until it dominates from ''Z'' = 125, and the proton [[nuclear drip line|drip line]] around ''Z'' = 130. The white rings denote the expected location of the island of stability; the two squares outlined in white denote 291[[copernicium|Cn]] and 293Cn, predicted to be the longest-lived nuclides on the island with half-lives of centuries or millennia.<ref name=Karpov /> The black square near the bottom of the second picture is [[uranium-238]], the heaviest confirmed [[primordial nuclide]] (a nuclide stable enough to have survived from the Earth's formation to the present day).
}}

====Magic numbers and the island of stability====
The stability of nuclei decreases greatly with the increase in atomic number after [[curium]], element 96, so that all isotopes with an atomic number above [[mendelevium|101]] [[radioactive decay|decay radioactively]] with a [[half-life]] under a day. No elements with [[atomic number]]s above 82 (after [[lead]]) have stable isotopes.<ref>{{cite journal|last = Marcillac|first = Pierre de |author2= Noël Coron|author3= Gérard Dambier|author4= Jacques Leblanc|author5= Jean-Pierre Moalic|date=April 2003|title = Experimental detection of α-particles from the radioactive decay of natural bismuth|journal = Nature|volume = 422|pages = 876–878|pmid=12712201|doi = 10.1038/nature01541|issue = 6934|bibcode = 2003Natur.422..876D|s2cid = 4415582 }}</ref> Nevertheless, because of [[magic number (physics)|reasons]] not very well understood yet, there is a slight increased nuclear stability around atomic numbers [[darmstadtium|110]]–[[flerovium|114]], which leads to the appearance of what is known in nuclear physics as the "[[island of stability]]". This concept, proposed by [[University of California, Berkeley|University of California]] professor [[Glenn Seaborg]], explains why [[superheavy element]]s last longer than predicted.<ref>{{cite book|title=Van Nostrand's scientific encyclopedia|first1=Glenn D. |last1= Considine |first2=Peter H. |last2= Kulik|publisher=Wiley-Interscience |year=2002|edition=9|isbn=978-0-471-33230-5|oclc=223349096}}</ref>

Calculations according to the [[Hartree–Fock method|Hartree–Fock–Bogoliubov method]] using the non-relativistic [[Skyrme interaction]] have proposed ''Z''&nbsp;=&nbsp;126 as a [[nuclear shell model|closed proton shell]]. In this region of the periodic table, ''N''&nbsp;=&nbsp;184, ''N''&nbsp;=&nbsp;196, and ''N''&nbsp;=&nbsp;228 have been suggested as closed neutron shells. Therefore, the isotopes of most interest are 310126, 322126, and 354126, for these might be considerably longer-lived than other isotopes. Element 126, having a [[magic number (physics)|magic number]] of [[proton]]s, is predicted to be more stable than other elements in this region, and may have [[nuclear isomer]]s with very long [[half-life|half-lives]].<ref name="emsley2"/> It is also possible that the [[island of stability]] is instead centered at 306[[unbibium|122]], which may be spherical and [[doubly magic]].<ref name="Kratz"/> Probably, the island of stability occurs around ''Z''&nbsp;=&nbsp;114–126 and ''N''&nbsp;=&nbsp;184, with lifetimes probably around hours to days. Beyond the shell closure at ''N''&nbsp;=&nbsp;184, spontaneous fission lifetimes should drastically drop below 10−15 seconds – too short for a nucleus to obtain an electron cloud and participate in any chemistry. That being said, such lifetimes are very model-dependent, and predictions range across many orders of magnitude.<ref name=gamowstates/>

Taking nuclear deformation and relativistic effects into account, an analysis of single-particle levels predicts new magic numbers for superheavy nuclei at ''Z''&nbsp;=&nbsp;126, 138, 154, and 164 and ''N''&nbsp;=&nbsp;228, 308, and 318.<ref name=fossilfission>{{cite web|last1=Maly|first1=J.|last2=Walz|first2=D.R.|title=Search for superheavy elements among fossil fission tracks in zircon|date=1980|url=http://www.slac.stanford.edu/pubs/slacpubs/2500/slac-pub-2554.pdf|access-date=2018-12-07}}</ref><ref name=magickoura>{{cite journal|last1=Koura|first1=H.|last2=Chiba|first2=S.|date=2013|title=Single-Particle Levels of Spherical Nuclei in the Superheavy and Extremely Superheavy Mass Region|journal=Journal of the Physical Society of Japan|volume=82|issue=1|pages=014201|url=https://www.researchgate.net/publication/258799250 |doi=10.7566/JPSJ.82.014201|bibcode=2013JPSJ...82a4201K}}</ref> Therefore, in addition to the island of stability centered at 291Cn, 293Cn,<ref name=Zagrebaev /> and 298Fl, further islands of stability may exist around the doubly magic 354126 as well as 472164 or 482164.<ref name="eurekalert.org"/><ref name="link.springer.com"/> These nuclei are predicted to be [[beta-decay stable isobars|beta-stable]] and decay by alpha emission or spontaneous fission with relatively long half-lives, and confer additional stability on neighboring ''N''&nbsp;=&nbsp;228 [[isotone]]s and elements 152–168, respectively.<ref name=SHlimit>{{cite conference|last=Koura|first=H.|date=2011|title=Decay modes and a limit of existence of nuclei in the superheavy mass region|url=http://tan11.jinr.ru/pdf/10_Sep/S_2/05_Koura.pdf|conference=4th International Conference on the Chemistry and Physics of the Transactinide Elements|access-date=18 November 2018}}</ref> On the other hand, the same analysis suggests that proton shell closures may be relatively weak or even nonexistent in some cases such as 354126, meaning that such nuclei might not be doubly magic and stability will instead be primarily determined by strong neutron shell closures.<ref name=magickoura /> Additionally, due to the enormously greater forces of [[coulomb repulsion|electromagnetic repulsion]] that must be overcome by the strong force at the second island (''Z''&nbsp;=&nbsp;164),<ref name=greinernuclei>{{cite journal|last=Greiner|first=W.|date=2013|title=Nuclei: superheavy-superneutronic-strange-and of antimatter|url=http://inspirehep.net/record/1221632/files/jpconf13_413_012002.pdf|journal=Journal of Physics: Conference Series|volume=413|issue=1|pages=012002|doi=10.1088/1742-6596/413/1/012002|bibcode=2013JPhCS.413a2002G|doi-access=free}}</ref> it is possible that nuclei around this region only exist as [[resonance (particle physics)|resonances]] and cannot stay together for a meaningful amount of time. It is also possible that some of the superactinides between these series may not actually exist because they are too far from both islands,<ref name=greinernuclei /> in which case the periodic table might end around ''Z''&nbsp;=&nbsp;130.<ref name="BFricke"/> Interestingly, the area of elements 121–156 where periodicity is in abeyance is quite similar to the gap between the two islands.<ref name=primefan/>

Beyond element 164, the [[fissility]] line defining the limit of stability with respect to spontaneous fission may converge with the [[neutron drip line]], posing a limit to the existence of heavier elements.<ref name=SHlimit /> Nevertheless, further magic numbers have been predicted at ''Z''&nbsp;=&nbsp;210, 274, and 354 and ''N''&nbsp;=&nbsp;308, 406, 524, 644, and 772,<ref name=Denisov>{{cite journal|last=Denisov|first=V.|date=2005|title=Magic numbers of ultraheavy nuclei|journal=Physics of Atomic Nuclei|url= https://www.researchgate.net/publication/225734594|volume=68|issue=7|pages=1133–1137|doi=10.1134/1.1992567|bibcode=2005PAN....68.1133D|s2cid=119430168}}</ref> with two beta-stable doubly magic nuclei found at 616210 and 798274; the same calculation method reproduced the predictions for 298Fl and 472164. (The doubly magic nuclei predicted for ''Z''&nbsp;=&nbsp;354 are beta-unstable, with 998354 being neutron-deficient and 1126354 being neutron-rich.) Although additional stability toward alpha decay and fission are predicted for 616210 and 798274, with half-lives up to hundreds of microseconds for 616210,<ref name=Denisov /> there will not exist islands of stability as significant as those predicted at ''Z''&nbsp;=&nbsp;114 and 164. As the existence of superheavy elements is very strongly dependent on stabilizing effects from closed shells, nuclear instability and fission will likely determine the end of the periodic table beyond these islands of stability.<ref name="BFricke"/><ref name=limit146 /><ref name=SHlimit />

The International Union of Pure and Applied Chemistry (IUPAC) defines an element to exist if its lifetime is longer than 10−14 seconds, which is the time it takes for the nucleus to form an electron cloud. However, a [[nuclide]] is generally considered to exist if its lifetime is longer than about 10−22 seconds, which is the time it takes for [[nuclear structure]] to form. Consequently, it is possible that some ''Z'' values can only be realised in nuclides and that the corresponding elements do not exist.<ref name=colloq/>

It is also possible that no further islands actually exist beyond 126, as the nuclear shell structure gets smeared out (as the electron shell structure already is expected to be around oganesson) and low-energy decay modes become readily available.<ref name=relqed>{{cite journal |last1=Schwerdtfeger |first1=Peter |last2=Pašteka |first2=Lukáš F. |last3=Punnett |first3=Andrew |last4=Bowman |first4=Patrick O. |date=2015 |title=Relativistic and quantum electrodynamic effects in superheavy elements |journal=Nuclear Physics A |volume=944 |issue=December 2015 |pages=551–577 |doi=10.1016/j.nuclphysa.2015.02.005|bibcode=2015NuPhA.944..551S }}</ref>

In some regions of the table of nuclides, there are expected to be additional regions of stability due to non-spherical nuclei that have different magic numbers than spherical nuclei do; the egg-shaped 270[[Hassium|Hs]] {{nowrap|1=(''Z'' = 108, ''N'' = 162)}} is one such deformed doubly magic nucleus.<ref>{{cite journal|last1=Dvorak|first1=J.|last2=Brüchle|first2=W.|last3=Chelnokov|first3=M.|last4=Dressler|first4=R.|last5=Düllmann|first5=Ch. E.|last6=Eberhardt|first6=K.|last7=Gorshkov|first7=V.|last8=Jäger|first8=E.|last9=Krücken|first9=R.|last10=Kuznetsov|first10=A.|last11=Nagame|first11=Y.|last12=Nebel|first12=F.|last13=Novackova|first13=Z.|last14=Qin|first14=Z.|last15=Schädel|first15=M.|last16=Schausten|first16=B.|last17=Schimpf|first17=E.|last18=Semchenkov|first18=A.|last19=Thörle|first19=P.|last20=Türler|first20=A.|last21=Wegrzecki|first21=M.|last22=Wierczinski|first22=B.|last23=Yakushev|first23=A.|last24=Yeremin|first24=A.|title=Doubly Magic Nucleus 108270Hs162 |journal=Physical Review Letters|volume=97|issue=24|pages=242501|year=2006|doi=10.1103/PhysRevLett.97.242501|pmid=17280272|bibcode=2006PhRvL..97x2501D|url=https://www.dora.lib4ri.ch/psi/islandora/object/psi%3A16351}}</ref> In the superheavy region, the strong Coulomb repulsion of protons may cause some nuclei, including isotopes of oganesson, to assume a bubble shape in the ground state with a reduced central density of protons, unlike the roughly uniform distribution inside most smaller nuclei.<ref>{{cite journal |last1=LaForge |first1=Evan |last2=Price |first2=Will |last3=Rafelski |first3=Johann |title=Superheavy elements and ultradense matter |journal=The European Physical Journal Plus |date=15 September 2023 |volume=138 |issue=9 |page=812 |doi=10.1140/epjp/s13360-023-04454-8|arxiv=2306.11989 |bibcode=2023EPJP..138..812L }}</ref><ref>{{cite news |title=Physicists are pushing the periodic table to its limits {{!}} Science News |url=https://www.sciencenews.org/article/physics-periodic-table-future-superheavy-elements |access-date=25 December 2023 |date=27 February 2019}}</ref> Such a shape would have a very low fission barrier, however.<ref>{{cite journal |last1=Dechargé |first1=J. |last2=Berger |first2=J.-F. |last3=Girod |first3=M. |last4=Dietrich |first4=K. |title=Bubbles and semi-bubbles as a new kind of superheavy nuclei |journal=Nuclear Physics A |date=March 2003 |volume=716 |pages=55–86 |doi=10.1016/S0375-9474(02)01398-2|bibcode=2003NuPhA.716...55D }}</ref> Even heavier nuclei in some regions, such as 342136 and 466156, may instead become [[torus|toroidal]] or [[red blood cell]]-like in shape, with their own magic numbers and islands of stability, but they would also fragment easily.<ref>{{cite journal |last1=Agbemava |first1=S. E. |last2=Afanasjev |first2=A. V. |title=Hyperheavy spherical and toroidal nuclei: The role of shell structure |journal=Physical Review C |date=25 March 2021 |volume=103 |issue=3 |pages=034323 |doi=10.1103/PhysRevC.103.034323 |arxiv=2012.13799|bibcode=2021PhRvC.103c4323A }}</ref><ref>{{cite journal |last1=Afanasjev |first1=A.V. |last2=Agbemava |first2=S.E. |last3=Gyawali |first3=A. |title=Hyperheavy nuclei: Existence and stability |journal=Physics Letters B |date=July 2018 |volume=782 |pages=533–540 |doi=10.1016/j.physletb.2018.05.070|doi-access=free |arxiv=1804.06395 |bibcode=2018PhLB..782..533A }}</ref>

====Predicted decay properties of undiscovered elements====
As the main island of stability is thought to lie around 291Cn and 293Cn, undiscovered elements beyond [[oganesson]] may be very unstable and undergo [[alpha decay]] or [[spontaneous fission]] in microseconds or less. The exact region in which half-lives exceed one microsecond is unknown, though various models suggest that isotopes of elements heavier than [[unbinilium]] that may be produced in fusion reactions with available targets and projectiles will have half-lives under one microsecond and therefore may not be detected.<ref name=Karpov /> It is consistently predicted that there will exist regions of stability at ''N'' = 184 and ''N'' = 228, and possibly also at ''Z'' ~ 124 and ''N'' ~ 198. These nuclei may have half-lives of a few seconds and undergo predominantly alpha decay and spontaneous fission, though minor [[positron emission|beta-plus decay]] (or [[electron capture]]) branches may also exist.<ref name=Palenzuela>{{cite journal|last1=Palenzuela|first1=Y. M.|last2=Ruiz|first2=L. F.|last3=Karpov|first3=A.|last4=Greiner|first4=W.|year=2012|title=Systematic Study of Decay Properties of Heaviest Elements|journal=Bulletin of the Russian Academy of Sciences: Physics|volume=76|issue=11|pages=1165–1171|issn=1062-8738|url=http://nrv.jinr.ru/karpov/publications/Palenzuela12_BRAS.pdf|doi=10.3103/S1062873812110172|bibcode=2012BRASP..76.1165P|s2cid=120690838}}</ref> Outside these regions of enhanced stability, [[fission barrier]]s are expected to drop significantly due to loss of stabilization effects, resulting in fission half-lives below [[attosecond|10−18]] seconds, especially in [[even and odd atomic nuclei|even–even nuclei]] for which hindrance is even lower due to [[nucleon pair breaking in fission|nucleon pairing]].<ref name=SHlimit /> In general, alpha decay half-lives are expected to increase with neutron number, from nanoseconds in the most neutron-deficient isotopes to seconds closer to the [[beta-stability line]].<ref name="sciencedirect1" /> For nuclei with only a few neutrons more than a magic number, [[nuclear binding energy|binding energy]] substantially drops, resulting in a break in the trend and shorter half-lives.<ref name="sciencedirect1" /> The most neutron deficient isotopes of these elements may also be unbound and undergo [[proton emission]]. [[Cluster decay]] (heavy particle emission) has also been proposed as an alternative decay mode for some isotopes,<ref>{{cite journal |last1=Poenaru |first1=Dorin N. |last2=Gherghescu |first2=R. A. |last3=Greiner |first3=W. |date=2012 |title=Cluster decay of superheavy nuclei |url=https://www.researchgate.net/publication/235507943 |journal=Physical Review C |volume=85 |issue=3 |pages=034615 |doi=10.1103/PhysRevC.85.034615 |access-date=2 May 2017|bibcode=2012PhRvC..85c4615P }}</ref> posing yet another hurdle to identification of these elements.

===Electron configurations===
The following are expected electron configurations of elements 119–174 and 184. The symbol [Og] indicates the probable electron configuration of oganesson (Z = 118), which is currently the last known element. The configurations of the elements in this table are written starting with [Og] because oganesson is expected to be the last prior element with a closed-shell (inert gas) configuration, 1s2 2s2 2p6 3s2 3p6 3d10 4s2 4p6 4d10 4f14 5s2 5p6 5d10 5f14 6s2 6p6 6d10 7s2 7p6. Similarly, the [172] in the configurations for elements 173, 174, and 184 denotes the likely closed-shell configuration of element 172.

Beyond element 123, no complete calculations are available and hence the data in this table must be taken as [[wiktionary:tentative|tentative]].<ref name="BFricke"/><ref name="BFricke1977" /><ref name="E123-vdSchoor2011">{{cite thesis|last=van der Schoor|first=K.|title=Electronic structure of element 123|url=http://fse.studenttheses.ub.rug.nl/14531/1/report.pdf|date=2016|publisher=Rijksuniversiteit Groningen}}</ref> In the case of element 123, and perhaps also heavier elements, several possible electron configurations are predicted to have very similar energy levels, such that it is very difficult to predict the [[ground state]]. All configurations that have been proposed (since it was understood that the Madelung rule probably stops working here) are included.<ref name="E123-vdSchoor2011" /><ref name=Umemoto>{{cite journal |last1=Umemoto |first1=Koichiro |last2=Saito |first2=Susumu |date=1996 |title=Electronic Configurations of Superheavy Elements |url=https://journals.jps.jp/doi/pdf/10.1143/JPSJ.65.3175 |journal=Journal of the Physical Society of Japan |volume=65 |issue=10 |pages=3175–9 |doi=10.1143/JPSJ.65.3175 |bibcode=1996JPSJ...65.3175U |access-date=31 January 2021}}</ref><ref>{{Cite journal|url=https://link.springer.com/article/10.1007/s00214-010-0887-3|doi = 10.1007/s00214-010-0887-3|title = Are MCDF calculations 101% correct in the super-heavy elements range?|year = 2011|last1 = Indelicato|first1 = Paul|last2 = Bieroń|first2 = Jacek|last3 = Jönsson|first3 = Per|journal = Theoretical Chemistry Accounts|volume = 129|issue = 3–5|pages = 495–505|hdl = 2043/12984|s2cid = 54680128|hdl-access = free}}</ref>

The predicted block assignments up to 172 are Kulsha's,<ref name=dications>{{Cite web|url=http://www.primefan.ru/stuff/chem/ptable/dications.html|title = Feasible electron configurations of dications up to Z = 172|access-date=2021-07-04}}</ref> following the expected available valence orbitals. There is, however, not a consensus in the literature as to how the blocks should work after element 138.

:{| class="wikitable"
! colspan="3" | [[Chemical element]] !! [[Block (periodic table)|Block]] !! Predicted [[electron configuration]]s<ref name=Haire/><ref name="BFricke"/><ref name="BFricke1977"/><ref name=nefedov/>
|-bgcolor="{{element color|s-block}}"
|| 119 || '''Uue''' || [[Ununennium]] ||s-block ||[Og] 8s1
|-bgcolor="{{element color|s-block}}"
|| 120 || '''Ubn''' || [[Unbinilium]] ||s-block ||[Og] 8s2
|-bgcolor="{{element color|g-block}}"
|| 121 || '''Ubu''' || [[Unbiunium]] ||g-block || [Og] 8s2 8p{{su|p=1|b=1/2}}<ref name=Umemoto/>
|-bgcolor="{{element color|g-block}}"
|| 122 || '''Ubb''' || [[Unbibium]] ||g-block || [Og] 8s2 8p{{su|p=2|b=1/2}}<ref name=Umemoto/> [Og] 7d1 8s2 8p{{su|p=1|b=1/2}}
|-bgcolor="{{element color|g-block}}"
|| 123 || '''Ubt''' || Unbitrium ||g-block || [Og] 6f1 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig>{{cite web |url=http://www.primefan.ru/stuff/chem/ptable/ptable.html |title=Archived copy |website=www.primefan.ru |access-date=15 January 2022 |archive-url=https://web.archive.org/web/20160305034205/http://www.primefan.ru/stuff/chem/ptable/ptable.html |archive-date=5 March 2016 |url-status=dead}}</ref> [Og] 6f1 7d1 8s2 8p{{su|p=1|b=1/2}}<ref name="E123-vdSchoor2011"/><ref name=Umemoto/> [Og] 6f2 8s2 8p{{su|p=1|b=1/2}} [Og] 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=1|b=3/2}}<ref name="E123-vdSchoor2011"/>
|-bgcolor="{{element color|g-block}}"
|| 124 || '''Ubq''' || [[Unbiquadium]] ||g-block || [Og] 6f2 8s2 8p{{su|p=2|b=1/2}}<ref name=Umemoto/><ref name=econfig/> [Og] 6f3 8s2 8p{{su|p=1|b=1/2}}
|-bgcolor="{{element color|g-block}}"
|| 125 || '''Ubp''' || Unbipentium ||g-block || [Og] 6f4 8s2 8p{{su|p=1|b=1/2}}<ref name=Umemoto/> [Og] 5g1 6f2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 5g1 6f3 8s2 8p{{su|p=1|b=1/2}} [Og] 8s2 0.81(5g1 6f2 8p{{su|p=2|b=1/2}}) + 0.17(5g1 6f1 7d2 8p{{su|p=1|b=1/2}}) + 0.02(6f3 7d1 8p{{su|p=1|b=1/2}})
|-bgcolor="{{element color|g-block}}"
|| 126 || '''Ubh''' || [[Unbihexium]] ||g-block || [Og] 5g1 6f4 8s2 8p{{su|p=1|b=1/2}}<ref name=Umemoto/> [Og] 5g2 6f2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 5g2 6f3 8s2 8p{{su|p=1|b=1/2}} [Og] 8s2 0.998(5g2 6f3 8p{{su|p=1|b=1/2}}) + 0.002(5g2 6f2 8p{{su|p=2|b=1/2}})
|-bgcolor="{{element color|g-block}}"
|| 127 || '''Ubs''' || Unbiseptium ||g-block || [Og] 5g2 6f3 8s2 8p{{su|p=2|b=1/2}}<ref name=Umemoto/> [Og] 5g3 6f2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 8s2 0.88(5g3 6f2 8p{{su|p=2|b=1/2}}) + 0.12(5g3 6f1 7d2 8p{{su|p=1|b=1/2}})
|-bgcolor="{{element color|g-block}}"
|| 128 || '''Ubo''' ||Unbioctium||g-block || [Og] 5g3 6f3 8s2 8p{{su|p=2|b=1/2}}<ref name=Umemoto/> [Og] 5g4 6f2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 8s2 0.88(5g4 6f2 8p{{su|p=2|b=1/2}}) + 0.12(5g4 6f1 7d2 8p{{su|p=1|b=1/2}})
|-bgcolor="{{element color|g-block}}"
|| 129 || '''Ube''' || Unbiennium ||g-block || [Og] 5g4 6f3 7d1 8s2 8p{{su|p=1|b=1/2}} [Og] 5g4 6f3 8s2 8p{{su|p=2|b=1/2}}<ref name=Umemoto/><ref name=econfig/> [Og] 5g5 6f2 8s2 8p{{su|p=2|b=1/2}} [Og] 5g4 6f3 7d1 8s2 8p{{su|p=1|b=1/2}}
|-bgcolor="{{element color|g-block}}"
|| 130 || '''Utn''' || Untrinilium ||g-block || [Og] 5g5 6f3 7d1 8s2 8p{{su|p=1|b=1/2}} [Og] 5g5 6f3 8s2 8p{{su|p=2|b=1/2}}<ref name=Umemoto/><ref name=econfig/> [Og] 5g6 6f2 8s2 8p{{su|p=2|b=1/2}} [Og] 5g5 6f3 7d1 8s2 8p{{su|p=1|b=1/2}}
|-bgcolor="{{element color|g-block}}"
|| 131 || '''Utu''' || Untriunium ||g-block || [Og] 5g6 6f3 8s2 8p{{su|p=2|b=1/2}}<ref name=Umemoto/><ref name=econfig/> [Og] 5g7 6f2 8s2 8p{{su|p=2|b=1/2}} [Og] 8s2 0.86(5g6 6f3 8p{{su|p=2|b=1/2}}) + 0.14(5g6 6f2 7d2 8p{{su|p=1|b=1/2}})
|-bgcolor="{{element color|g-block}}"
|| 132 || '''Utb''' || Untribium ||g-block || [Og] 5g7 6f3 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 5g8 6f2 8s2 8p{{su|p=2|b=1/2}}
|-bgcolor="{{element color|g-block}}"
|| 133 || '''Utt''' || Untritrium ||g-block || [Og] 5g8 6f3 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|g-block}}"
|| 134 || '''Utq''' || Untriquadium ||g-block || [Og] 5g8 6f4 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|g-block}}"
|| 135 || '''Utp''' || Untripentium ||g-block || [Og] 5g9 6f4 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|g-block}}"
|| 136 || '''Uth''' || Untrihexium ||g-block || [Og] 5g10 6f4 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|g-block}}"
|| 137 || '''Uts''' || Untriseptium ||g-block || [Og] 5g11 6f4 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|g-block}}"
|| 138 || '''Uto''' || Untrioctium ||g-block || [Og] 5g12 6f4 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 5g12 6f3 7d1 8s2 8p{{su|p=2|b=1/2}}
|-bgcolor="{{element color|g-block}}"
|| 139 || '''Ute''' || Untriennium ||g-block || [Og] 5g13 6f3 7d1 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 5g13 6f2 7d2 8s2 8p{{su|p=2|b=1/2}}
|-bgcolor="{{element color|g-block}}"
|| 140 || '''Uqn''' || Unquadnilium ||g-block || [Og] 5g14 6f3 7d1 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 5g15 6f1 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=2|b=3/2}}
|-bgcolor="{{element color|g-block}}"
|| 141 || '''Uqu''' || Unquadunium ||g-block || [Og] 5g15 6f2 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|g-block}}"
|| 142 || '''Uqb''' || Unquadbium ||g-block || [Og] 5g16 6f2 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 143 || '''Uqt''' || Unquadtrium ||f-block || [Og] 5g17 6f2 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 144 || '''Uqq''' || Unquadquadium ||f-block || [Og] 5g18 6f2 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/> [Og] 5g18 6f1 7d3 8s2 8p{{su|p=2|b=1/2}} [Og] 5g17 6f2 7d3 8s2 8p{{su|p=2|b=1/2}} [Og] 8s2 0.95(5g17 6f2 7d3 8p{{su|p=2|b=1/2}}) + 0.05(5g17 6f4 7d1 8p{{su|p=2|b=1/2}})
|-bgcolor="{{element color|f-block}}"
|| 145 || '''Uqp''' || Unquadpentium ||f-block || [Og] 5g18 6f3 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 146 || '''Uqh''' || Unquadhexium ||f-block || [Og] 5g18 6f4 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 147 || '''Uqs''' || Unquadseptium ||f-block || [Og] 5g18 6f5 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 148 || '''Uqo''' || Unquadoctium ||f-block || [Og] 5g18 6f6 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 149 || '''Uqe''' || Unquadennium ||f-block || [Og] 5g18 6f6 7d3 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 150 || '''Upn''' || Unpentnilium ||f-block || [Og] 5g18 6f6 7d4 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f7 7d3 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 151 || '''Upu''' || Unpentunium ||f-block || [Og] 5g18 6f8 7d3 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 152 || '''Upb''' || Unpentbium ||f-block || [Og] 5g18 6f9 7d3 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 153 || '''Upt''' || Unpenttrium ||f-block || [Og] 5g18 6f10 7d3 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f11 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 154 || '''Upq''' || Unpentquadium ||f-block || [Og] 5g18 6f11 7d3 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f12 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 155 || '''Upp''' || Unpentpentium ||f-block || [Og] 5g18 6f12 7d3 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f13 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|f-block}}"
|| 156 || '''Uph''' || Unpenthexium ||f-block|| [Og] 5g18 6f13 7d3 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d2 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 157 || '''Ups''' || Unpentseptium ||d-block || [Og] 5g18 6f14 7d3 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 158 || '''Upo''' || Unpentoctium ||d-block || [Og] 5g18 6f14 7d4 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 159 || '''Upe''' || Unpentennium ||d-block || [Og] 5g18 6f14 7d5 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d4 8s2 8p{{su|p=2|b=1/2}} 9s1<ref name=econfig/>
|-bgcolor="{{element color|d-block}}" {{Anchor|Uhn|Unhexnilium}}
|| 160 || '''Uhn''' || Unhexnilium ||d-block || [Og] 5g18 6f14 7d6 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d5 8s2 8p{{su|p=2|b=1/2}} 9s1<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 161 || '''Uhu''' || Unhexunium ||d-block || [Og] 5g18 6f14 7d7 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d6 8s2 8p{{su|p=2|b=1/2}} 9s1<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 162 || '''Uhb''' || Unhexbium ||d-block || [Og] 5g18 6f14 7d8 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d7 8s2 8p{{su|p=2|b=1/2}} 9s1<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 163 || '''Uht''' || Unhextrium ||d-block || [Og] 5g18 6f14 7d9 8s2 8p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d8 8s2 8p{{su|p=2|b=1/2}} 9s1<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 164 || '''Uhq''' || Unhexquadium ||d-block || [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 165 || '''Uhp''' || Unhexpentium ||d-block || [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 9s1<ref name=econfig/>
|-bgcolor="{{element color|d-block}}"
|| 166 || '''Uhh''' || Unhexhexium ||d-block ||[Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 9s2<ref name=econfig/>
|-bgcolor="{{element color|p-block}}"
|| 167 || '''Uhs''' || Unhexseptium ||p-block || [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 9s2 9p{{su|p=1|b=1/2}} [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=1|b=3/2}} 9s2<ref name=econfig/>
|-bgcolor="{{element color|p-block}}"
|| 168 || '''Uho''' || Unhexoctium ||p-block || [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 9s2 9p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=2|b=3/2}} 9s2<ref name=econfig/>
|-bgcolor="{{element color|p-block}}"
|| 169 || '''Uhe''' || Unhexennium ||p-block || [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=1|b=3/2}} 9s2 9p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=3|b=3/2}} 9s2<ref name=econfig/>
|-bgcolor="{{element color|p-block}}"
|| 170 || '''Usn''' || Unseptnilium ||p-block || [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=2|b=3/2}} 9s2 9p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=4|b=3/2}} 9s2<ref name=econfig/>
|-bgcolor="{{element color|p-block}}"
|| 171 || '''Usu''' || Unseptunium ||p-block || [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=3|b=3/2}} 9s2 9p{{su|p=2|b=1/2}} [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=4|b=3/2}} 9s2 9p{{su|p=1|b=1/2}}<ref name=econfig/>
|-bgcolor="{{element color|p-block}}"
|| 172 || '''{{Not a typo|Usb}}''' || Unseptbium ||p-block || [Og] 5g18 6f14 7d10 8s2 8p{{su|p=2|b=1/2}} 8p{{su|p=4|b=3/2}} 9s2 9p{{su|p=2|b=1/2}}<ref name=econfig/>
|-
|| 173 || '''Ust''' || Unsepttrium || ? || [172] 6g1 [172] 9p{{su|p=1|b=3/2}} [172] 10s1<ref name=eliav2023>{{cite web |url=https://indico.jinr.ru/event/3622/contributions/20027/attachments/15317/25832/Ephraim%20Eliav%20Yerevan-2023F.pptx |title=Benchmark atomic electronic structures calculations at the edge of Periodic Table |last=Eliav |first=Ephraim |date=26 April 2023 |website=jinr.ru |publisher=JINR |access-date=29 July 2023 |quote=}}</ref>
|-
|| 174 || '''Usq''' || Unseptquadium || ? || [172] 8d1 10s1<ref name=eliav2023/>
|-
|| ... || ... || ... || ... || ...
|-
|| 184 || '''Uoq''' || Unoctquadium || ? || [172] 6g5 7f4 8d3
|}

==See also==
* [[Table of nuclides]]
* [[Hypernucleus]]
* [[Neutronium]]

==References==
{{reflist}}

==Further reading==
* {{Cite book | last1 = Kaldor | first1 = U. | chapter = Superheavy Elements—Chemistry and Spectroscopy | doi = 10.1002/0470845015.cu0044 | title = Encyclopedia of Computational Chemistry | year = 2005 | isbn = 978-0470845011 }}
* {{Cite journal | last1 = Seaborg | first1 = G. T. | doi = 10.1146/annurev.ns.18.120168.000413| doi-access=free | title = Elements Beyond 100, Present Status and Future Prospects | journal = [[Annual Review of Nuclear Science]] | volume = 18 | pages = 53–152| year = 1968 |bibcode = 1968ARNPS..18...53S }}
* {{Cite book | last1 = Scerri | first1 = Eric. | title = A Very Short Introduction to the Periodic Table, Oxford University Press, Oxford | year = 2011 | publisher = OUP Oxford | isbn = 978-0-19-958249-5 }}

==External links==
* {{cite web|url=http://www.uky.edu/~holler/html/g.html|title= Images of g-orbitals|publisher=University of Kentucky|first=Jim|last= Holler|archive-url= https://web.archive.org/web/20160303225243/http://www.uky.edu/~holler/html/g.html|access-date=2016-03-03|archive-date= 2016-03-03}}
* {{Cite web|url=http://jeries.rihani.com |title= The extended periodic table of the elements| first1 = Jeries A.|last1=Rihani|access-date=2009-02-02}}
* {{Cite web|url=http://www.ericscerri.com |title= Eric Scerri's website for the elements and the periodic table|first1=Eric |last1=Scerri|access-date=2013-03-26}}

[[Category:Hypothetical chemical elements|*]]
[[Category:Periodic table]]
[[Category:Nuclear physics]]

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Latin: A a Á á À à Â â Ä ä Ǎ ǎ Ă ă Ā ā Ã ã Å å Ą ą Æ æ Ǣ ǣ B b C c Ć ć Ċ ċ Ĉ ĉ Č č Ç ç D d Ď ď Đ đ Ḍ ḍ Ð ð E e É é È è Ė ė Ê ê Ë ë Ě ě Ĕ ĕ Ē ē Ẽ ẽ Ę ę Ẹ ẹ Ɛ ɛ Ǝ ǝ Ə ə F f G g Ġ ġ Ĝ ĝ Ğ ğ Ģ ģ H h Ĥ ĥ Ħ ħ Ḥ ḥ I i İ ı Í í Ì ì Î î Ï ï Ǐ ǐ Ĭ ĭ Ī ī Ĩ ĩ Į į Ị ị J j Ĵ ĵ K k Ķ ķ L l Ĺ ĺ Ŀ ŀ Ľ ľ Ļ ļ Ł ł Ḷ ḷ Ḹ ḹ M m Ṃ ṃ N n Ń ń Ň ň Ñ ñ Ņ ņ Ṇ ṇ Ŋ ŋ O o Ó ó Ò ò Ô ô Ö ö Ǒ ǒ Ŏ ŏ Ō ō Õ õ Ǫ ǫ Ọ ọ Ő ő Ø ø Œ œ Ɔ ɔ P p Q q R r Ŕ ŕ Ř ř Ŗ ŗ Ṛ ṛ Ṝ ṝ S s Ś ś Ŝ ŝ Š š Ş ş Ș ș Ṣ ṣ ß T t Ť ť Ţ ţ Ț ț Ṭ ṭ Þ þ U u Ú ú Ù ù Û û Ü ü Ǔ ǔ Ŭ ŭ Ū ū Ũ ũ Ů ů Ų ų Ụ ụ Ű ű Ǘ ǘ Ǜ ǜ Ǚ ǚ Ǖ ǖ V v W w Ŵ ŵ X x Y y Ý ý Ŷ ŷ Ÿ ÿ Ỹ ỹ Ȳ ȳ Z z Ź ź Ż ż Ž ž ß Ð ð Þ þ Ŋ ŋ Ə ə
Greek: Ά ά Έ έ Ή ή Ί ί Ό ό Ύ ύ Ώ ώ Α α Β β Γ γ Δ δ Ε ε Ζ ζ Η η Θ θ Ι ι Κ κ Λ λ Μ μ Ν ν Ξ ξ Ο ο Π π Ρ ρ Σ σ ς Τ τ Υ υ Φ φ Χ χ Ψ ψ Ω ω {{Polytonic|}}
Cyrillic: А а Б б В в Г г Ґ ґ Ѓ ѓ Д д Ђ ђ Е е Ё ё Є є Ж ж З з Ѕ ѕ И и І і Ї ї Й й Ј ј К к Ќ ќ Л л Љ љ М м Н н Њ њ О о П п Р р С с Т т Ћ ћ У у Ў ў Ф ф Х х Ц ц Ч ч Џ џ Ш ш Щ щ Ъ ъ Ы ы Ь ь Э э Ю ю Я я ́
IPA: t̪ d̪ ʈ ɖ ɟ ɡ ɢ ʡ ʔ ɸ β θ ð ʃ ʒ ɕ ʑ ʂ ʐ ç ʝ ɣ χ ʁ ħ ʕ ʜ ʢ ɦ ɱ ɳ ɲ ŋ ɴ ʋ ɹ ɻ ɰ ʙ ⱱ ʀ ɾ ɽ ɫ ɬ ɮ ɺ ɭ ʎ ʟ ɥ ʍ ɧ ʼ ɓ ɗ ʄ ɠ ʛ ʘ ǀ ǃ ǂ ǁ ɨ ʉ ɯ ɪ ʏ ʊ ø ɘ ɵ ɤ ə ɚ ɛ œ ɜ ɝ ɞ ʌ ɔ æ ɐ ɶ ɑ ɒ ʰ ʱ ʷ ʲ ˠ ˤ ⁿ ˡ ˈ ˌ ː ˑ ̪ {{IPA|}}

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