m →References: Journal cites, added 1 DOI, added 1 Bibcode using AWB (10499)
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Rescuing 2 sources and tagging 0 as dead.) #IABot (v2.0.9.5
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{{Short description|Star in the constellation Ara}} |
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:''Not to be confused with [[Gliese 674]].'' |
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⚫ | |||
⚫ | | name = [[Gliese Catalogue of Nearby Stars|Gliese]] 676 A/B |
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⚫ | |||
⚫ |
| name = [[Gliese Catalogue of Nearby Stars|Gliese]] 676 A/B |
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}} |
}} |
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{{Starbox observe |
{{Starbox observe |
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| epoch = J2000.0 |
| epoch = J2000.0 |
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| constell = [[Ara (constellation)|Ara]] |
| constell = [[Ara (constellation)|Ara]] |
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Line 10: | Line 9: | ||
| dec = {{DEC|–51|38|13.1}}<ref name="van Leeuwen2007"/> |
| dec = {{DEC|–51|38|13.1}}<ref name="van Leeuwen2007"/> |
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| appmag_v = 9.59 |
| appmag_v = 9.59 |
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}} |
}} |
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{{Starbox character |
{{Starbox character |
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| class = M0V/M3V |
| class = M0V<ref name=mnras452_3_2745/>/M3V |
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| appmag_1_passband = B |
| appmag_1_passband = B |
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| appmag_1 = 11.05/14.8 |
| appmag_1 = 11.05/14.8 |
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| appmag_4_passband = K |
| appmag_4_passband = K |
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| appmag_4 = 5.825 |
| appmag_4 = 5.825 |
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| r-i = |
| r-i = |
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| v-r = |
| v-r = |
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| b-v = 1.46 |
| b-v = 1.46 |
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| u-b = |
| u-b = |
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| variable = |
| variable = |
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}} |
}} |
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{{Starbox astrometry |
{{Starbox astrometry |
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| radial_v = |
| radial_v = {{val|-39.82|0.14}}<ref name="GaiaDR3"/> |
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| prop_mo_ra = - |
| prop_mo_ra = {{val|-258.759|0.034}}<ref name="GaiaDR3"/> |
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| prop_mo_dec = - |
| prop_mo_dec = {{val|-185.119|0.025}}<ref name="GaiaDR3"/> |
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| parallax = |
| parallax = 62.5786 |
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| p_error = |
| p_error = 0.0303 |
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| parallax_footnote = <ref name=" |
| parallax_footnote = <ref name="GaiaDR3">{{Cite Gaia DR3|5925209583053212800}}</ref> |
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| absmag_v = 8.55 |
| absmag_v = 8.55 |
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}} |
}} |
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{{Starbox detail |
{{Starbox detail |
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| mass = 0. |
| mass = {{val|0.631|0.017}}<ref name="Pineda2021"/>/0.29<ref name="Forveille2011"/> |
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| radius = {{val|0.617|0.028|0.027}}<ref name="Pineda2021"/> |
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| radius = |
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| gravity = |
| gravity = |
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| luminosity = 0. |
| luminosity = 0.08892{{±|0.00220}}<ref name="Pineda2021"/> |
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| temperature = |
| temperature = {{val|4014|94|90|fmt=commas}}<ref name="Pineda2021"/> |
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| metal_fe = 0.23 |
| metal_fe = {{val|0.23|0.10}}<ref name="Forveille2011"/> |
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| age = |
| age = |
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| rotation = |
| rotation = {{val|41.2|3.8|u=d}}<ref name=mnras452_3_2745/> |
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}} |
}} |
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{{Starbox catalog |
{{Starbox catalog |
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| names = [[Durchmusterung|CD]]–51°10924, [[Hipparcos catalogue|HIP]] 85647, [[Luyten Two-Tenths catalogue|LTT]] 6947/6948, [[New Luyten Two-Tenths catalogue|NLTT]] 44859, [[New Suspected Variable catalog|NSV]] 8846 |
| names = [[Durchmusterung|CD]]–51°10924, [[Hipparcos catalogue|HIP]] 85647, [[Luyten Two-Tenths catalogue|LTT]] 6947/6948, [[New Luyten Two-Tenths catalogue|NLTT]] 44859, [[New Suspected Variable catalog|NSV]] 8846 |
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}} |
}} |
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==Planetary system== |
==Planetary system== |
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The first planet discovered, b, is a super-jovian first characterised in October 2009. The planet was formally announced in 2011,<ref name="Forveille2011"/> along with the first recognition of a trend not attributable to the companion star. Even after fitting a planet and a trend, it was noted that the residual velocities were still around 3.4 m/s, significantly larger than the instrumental errors of around 1.7 m/s. This tentatively implied the existence of other bodies in orbit, though nothing more could be said at the time.<ref name="Forveille2011"/> |
The first planet discovered, b, is a super-jovian first characterised in October 2009. The planet was formally announced in 2011,<ref name="Forveille2011"/> along with the first recognition of a trend not attributable to the companion star. Even after fitting a planet and a trend, it was noted that the residual velocities were still around 3.4 m/s, significantly larger than the instrumental errors of around 1.7 m/s. This tentatively implied the existence of other bodies in orbit, though nothing more could be said at the time.<ref name="Forveille2011"/> |
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Line 65: | Line 63: | ||
|last =Anglada-Escudé |first=Guillem |
|last =Anglada-Escudé |first=Guillem |
||
|author2=Butler, R. Paul |
|author2=Butler, R. Paul |
||
| |
|date = 2012 |
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|title = The HARPS-TERRA Project. I. Description of the Algorithms, Performance, and New Measurements on a Few Remarkable Stars Observed by HARPS |
|title = The HARPS-TERRA Project. I. Description of the Algorithms, Performance, and New Measurements on a Few Remarkable Stars Observed by HARPS |
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|arxiv = 1202.2570 |
|arxiv = 1202.2570 |
||
|bibcode = 2012ApJS..200...15A |
|bibcode = 2012ApJS..200...15A |
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|doi = 10.1088/0067-0049/200/2/15 |
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⚫ |
|
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|volume=200 |
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|journal=The Astrophysical Journal Supplement Series |
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|issue=2 |
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|pages=15|s2cid=118528839 |
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⚫ | }}</ref> Even with significantly lower margins of error on the data, less data was accessible than what was used in 2011. Still, the team reached a very similar conclusion to the previous team with a model of a planet and a trend. The residual velocities were still somewhat excessive, giving more weight to the existence of other bodies in the system, though still no conclusions could be made. |
||
Between the time of the previous analysis and June 2012, the rest of the radial-velocity measurements used in 2011 were made public,<ref name="4-planet"/> allowing them to be reduced using HARPS-TERRA. These were then analysed via a [[Bayesian probability]] analysis, which was previously used to discover [[HD 10180]] i and j, which confirmed planet b and made a first characterisation of planet c, which was previously only described as a trend. After the first two signals were introduced, the next most powerful signal was at around 35.5 days, with an analytic false alarm probability of 0.156. Through 10<sup>4</sup> trials, the false alarm probability was found to be 0.44%, low enough for it to be included as a periodic, planetary signal. With a minimum mass of around 11 |
Between the time of the previous analysis and June 2012, the rest of the radial-velocity measurements used in 2011 were made public,<ref name="4-planet"/> allowing them to be reduced using HARPS-TERRA. These were then analysed via a [[Bayesian probability]] analysis, which was previously used to discover [[HD 10180]] i and j, which confirmed planet b and made a first characterisation of planet c,<ref name=Sahlmann2016>{{citation|arxiv=1608.00918|year=2016|title=The mass of planet GJ 676A b from ground-based astrometry|doi=10.1051/0004-6361/201628854 |last1=Sahlmann |first1=J. |last2=Lazorenko |first2=P. F. |last3=Ségransan |first3=D. |last4=Astudillo-Defru |first4=N. |last5=Bonfils |first5=X. |last6=Delfosse |first6=X. |last7=Forveille |first7=T. |last8=Hagelberg |first8=J. |last9=Lo Curto |first9=G. |last10=Pepe |first10=F. |last11=Queloz |first11=D. |last12=Udry |first12=S. |last13=Zimmerman |first13=N. T. |journal=Astronomy & Astrophysics |volume=595 |pages=A77 |s2cid=118480445 }}</ref> which was previously only described as a trend. After the first two signals were introduced, the next most powerful signal was at around 35.5 days, with an analytic false alarm probability of 0.156. Through 10<sup>4</sup> trials, the false alarm probability was found to be 0.44%, low enough for it to be included as a periodic, planetary signal. With a minimum mass of around 11 Earths, the planet lies at the accepted border between [[Super-Earth]]s and gaseous, Neptune-like bodies of 10 Earths. |
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After accepting the third signal, a strong peak at 3.6 days became apparent. With a false alarm probability much lower than that of the previously accepted body, it was immediately accepted. With a minimum mass of around 4.5 |
After accepting the third signal, a strong peak at 3.6 days became apparent. With a false alarm probability much lower than that of the previously accepted body, it was immediately accepted. With a minimum mass of around 4.5 Earths, it is a small Super-Earth. |
||
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{{As of|2012}}, this system holds the record for the widest range of masses in a single planetary system,<ref name="4-planet"/> and also shows a hierarchy reminiscent of the solar system, with the [[gas giant]]s at large distances from the star while the smaller bodies are much closer-in. |
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In 2016, the true mass of Gliese 676 Ab was measured via [[astrometry]].<ref name=Sahlmann2016/> A 2022 study revised this mass estimate, along with measuring the true mass of Gliese 676 Ac.<ref name="Feng2022"/> There are two Super-Jupiter planets: "b" with a period of 1051 days (2.9 years) and a mass of {{Jupiter mass|5.79|link=y}}, and "c" with a period of 13900 days (38.1 years) and a mass of {{Jupiter mass|13.49|link=y}}, which is at the borderline between planets and [[brown dwarf]]s.<ref name="Feng2022"/> |
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{{OrbitboxPlanet begin |
{{OrbitboxPlanet begin |
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| table_ref = <ref name="4-planet"/> |
| table_ref = <ref name="4-planet"/><ref name=Sahlmann2016/><ref name="Feng2022"/> |
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| name = Gliese 676 A |
| name = Gliese 676 A |
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}} |
}} |
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{{OrbitboxPlanet |
{{OrbitboxPlanet |
||
| exoplanet = d |
| exoplanet = d |
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| mass_earth = |
| mass_earth = ≥{{val|4.4|0.3}} |
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| period = 3. |
| period = {{val|3.6005|0.0002}} |
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| semimajor = 0.0413 |
| semimajor = {{val|0.0413|0.0014}} |
||
| eccentricity = 0. |
| eccentricity = {{val|0.262|0.090|0.101}} |
||
}} |
}} |
||
{{OrbitboxPlanet |
{{OrbitboxPlanet |
||
| exoplanet = e |
| exoplanet = e |
||
| mass_earth = |
| mass_earth = ≥{{val|8.1|0.7}} |
||
| period = 35. |
| period = {{val|35.39|0.03|0.04}} |
||
| semimajor = 0.187 |
| semimajor = {{val|0.187|0.007}} |
||
| eccentricity = 0. |
| eccentricity = {{val|0.125|0.119|0.087}} |
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}} |
}} |
||
{{OrbitboxPlanet |
{{OrbitboxPlanet |
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| exoplanet = b |
| exoplanet = b |
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| mass = |
| mass = {{val|5.792|0.469|0.477}} |
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| period = |
| period = {{val|1051.4|0.4}} |
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| semimajor = 1. |
| semimajor = {{val|1.735|0.056|0.060}} |
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| eccentricity = 0. |
| eccentricity = {{val|0.319|0.003}} |
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| inclination = {{val|48.919|3.312|2.781}} |
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}} |
}} |
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{{OrbitboxPlanet |
{{OrbitboxPlanet |
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| exoplanet = c |
| exoplanet = c |
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| mass = |
| mass = {{val|13.492|1.046|1.127}} |
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| period = |
| period = {{val|13921.4|1238.4|1518.2}} |
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| semimajor = |
| semimajor = {{val|9.726|0.629|0.793}} |
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| eccentricity = 0. |
| eccentricity = {{val|0.295|0.033|0.049}} |
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| inclination = {{val|33.690|1.362|1.324}} |
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}} |
}} |
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{{Orbitbox end}} |
{{Orbitbox end}} |
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== References == |
== References == |
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{{Reflist |
{{Reflist|refs= |
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<ref name="Pineda2021">{{cite journal | title=The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars | last1=Pineda | first1=J. Sebastian | last2=Youngblood | first2=Allison | last3=France | first3=Kevin | journal=The Astrophysical Journal | volume=918 | issue=1 | id=40 | pages=23 | date=September 2021 | doi=10.3847/1538-4357/ac0aea | arxiv=2106.07656 | bibcode=2021ApJ...918...40P | s2cid=235435757 | doi-access=free }}</ref> |
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<ref name="4-planet">{{cite journal |
<ref name="4-planet">{{cite journal |
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|last |
|last=Anglada-Escudé |
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|first=Guillem |
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|author2=Tuomi, Mikko |
|author2=Tuomi, Mikko |
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| |
|date=2012 |
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|title |
|title=A planetary system with gas giants and super-Earths around the nearby M dwarf GJ 676A. Optimizing data analysis techniques for the detection of multi-planetary systems |
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|arxiv |
|arxiv=1206.7118 |
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|bibcode |
|bibcode=2012A&A...548A..58A |
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|doi=10.1051/0004-6361/201219910 |
|doi=10.1051/0004-6361/201219910 |
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|volume=548 |
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⚫ | |||
|journal=Astronomy |
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|pages=A58 |
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|s2cid=17115882 |
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|url=http://goedoc.uni-goettingen.de/goescholar/bitstream/handle/1/9595/aa19910-12.pdf?sequence=2 |
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}}{{Dead link|date=September 2023 |bot=InternetArchiveBot |fix-attempted=yes }}</ref> |
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<ref name="Forveille2011">{{ |
<ref name="Forveille2011">{{Cite journal |doi=10.1051/0004-6361/201016034 |last1=Forveille |first1=Thierry |last2=Bonfils |first2=Xavier |last3=LoCurto |first3=Gaspare |last4=Delfosse |first4=Xavier |last5=Udry |first5=Stéphane |last6=Bouchy |first6=François |last7=Lovis |first7=Christophe |last8=Mayor |first8=Michel |last9=Moutou |first9=Claire |last10=Naef |first10=Dominique |last11=Pepe |first11=Francesco |date=February 2011 |title=The HARPS search for southern extra-solar planets: XXVIII. Two giant planets around M0 dwarfs |arxiv=1012.1168 |journal=Astronomy & Astrophysics |volume=526 |pages=A141 |bibcode=2011A&A...526A.141F |issn=0004-6361 |doi-access=free }}</ref> |
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<ref name="van Leeuwen2007">{{cite journal | title=Validation of the new Hipparcos reduction | url=http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL | last1=van Leeuwen | first1=F. | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | |
<ref name="van Leeuwen2007">{{cite journal | title=Validation of the new Hipparcos reduction | url=http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL | last1=van Leeuwen | first1=F. | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | date=2007 | arxiv=0708.1752 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | s2cid=18759600 | access-date=2012-11-04 | archive-date=2019-12-07 | archive-url=https://web.archive.org/web/20191207150403/http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL | url-status=live }} [http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=85368 Vizier catalog entry ] {{Webarchive|url=https://web.archive.org/web/20220531095125/http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I%2F311%2Fhip2&recno=85368 |date=2022-05-31 }}</ref> |
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<ref name=mnras452_3_2745>{{citation |
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| display-authors=1 |
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| last1=Suárez Mascareño | first1=A. | last2=Rebolo | first2=R. |
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| last3=González Hernández | first3=J. I. | last4=Esposito | first4=M. |
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| title=Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators |
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| journal=Monthly Notices of the Royal Astronomical Society |
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| volume=452 | issue=3 | pages=2745–2756 | date=September 2015 |
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| doi=10.1093/mnras/stv1441 | bibcode=2015MNRAS.452.2745S |
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| arxiv=1506.08039 | s2cid=119181646 | postscript=. |
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⚫ | |||
<ref name="Feng2022">{{cite journal |last1=Feng |first1=Fabo |last2=Butler |first2=R. Paul |display-authors=etal |date=August 2022 |title=3D Selection of 167 Substellar Companions to Nearby Stars |journal=[[The Astrophysical Journal Supplement Series]] |volume=262 |issue=21 |page=21 |doi=10.3847/1538-4365/ac7e57 |arxiv=2208.12720 |bibcode=2022ApJS..262...21F|s2cid=251864022 |doi-access=free }}</ref> |
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}} |
}} |
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{{Sky|17|30|11.2042|-|51|38|13.116|52.6}} |
{{Sky|17|30|11.2042|-|51|38|13.116|52.6}} |
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{{Nearest star systems|11}} |
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{{Stars of Ara}} |
{{Stars of Ara}} |
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{{2012 in space}} |
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{{DEFAULTSORT:Gliese 676}} |
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[[Category:M-type main-sequence stars]] |
[[Category:M-type main-sequence stars]] |
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[[Category:Gliese and GJ objects|0676]] |
[[Category:Gliese and GJ objects|0676]] |
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[[Category:Planetary systems with four confirmed planets]] |
[[Category:Planetary systems with four confirmed planets]] |
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[[Category:Multi-star planetary systems|2]] |
[[Category:Multi-star planetary systems|2]] |
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[[Category: |
[[Category:Durchmusterung objects]] |
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[[Category:TIC objects]] |
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Ara |
Right ascension | 17h30m 11.20s[1] |
Declination | –51° 38′ 13.1″[1] |
Apparent magnitude (V) | 9.59 |
Characteristics | |
Spectral type | M0V[2]/M3V |
Apparent magnitude (B) | 11.05/14.8 |
Apparent magnitude (J) | 6.711 |
Apparent magnitude (H) | 6.082 |
Apparent magnitude (K) | 5.825 |
B−V color index | 1.46 |
Astrometry | |
Radial velocity (Rv) | −39.82±0.14[3] km/s |
Proper motion (μ) | RA: −258.759±0.034[3] mas/yr Dec.: −185.119±0.025[3] mas/yr |
Parallax (π) | 62.5786 ± 0.0303 mas[3] |
Distance | 52.12 ± 0.03 ly (15.980 ± 0.008 pc) |
Absolute magnitude (MV) | 8.55 |
Details | |
Mass | 0.631±0.017[4]/0.29[5] M☉ |
Radius | 0.617+0.028 −0.027[4] R☉ |
Luminosity | 0.08892±0.00220[4] L☉ |
Temperature | 4,014+94 −90[4] K |
Metallicity [Fe/H] | 0.23±0.10[5] dex |
Rotation | 41.2±3.8 d[2] |
Other designations | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
Gliese 676 is a 10th-magnitude wide binary systemofred dwarfs that has an estimated minimum separation of 800 AU with an orbital period of greater than 20,000 years.[6] It is located approximately 54 light years away in the constellation Ara. In 2009, a gas giant was found in orbit around the primary star, in addition to its confirmation in 2011 there was also a strong indication of a companion; the second gas giant was characterised in 2012, along with two much smaller planets.
The first planet discovered, b, is a super-jovian first characterised in October 2009. The planet was formally announced in 2011,[5] along with the first recognition of a trend not attributable to the companion star. Even after fitting a planet and a trend, it was noted that the residual velocities were still around 3.4 m/s, significantly larger than the instrumental errors of around 1.7 m/s. This tentatively implied the existence of other bodies in orbit, though nothing more could be said at the time.[5]
The star was a test case for the HARPS-TERRA software for better reduction of data from the HARPS spectrometer in early 2012.[7] Even with significantly lower margins of error on the data, less data was accessible than what was used in 2011. Still, the team reached a very similar conclusion to the previous team with a model of a planet and a trend. The residual velocities were still somewhat excessive, giving more weight to the existence of other bodies in the system, though still no conclusions could be made.
Between the time of the previous analysis and June 2012, the rest of the radial-velocity measurements used in 2011 were made public,[6] allowing them to be reduced using HARPS-TERRA. These were then analysed via a Bayesian probability analysis, which was previously used to discover HD 10180 i and j, which confirmed planet b and made a first characterisation of planet c,[8] which was previously only described as a trend. After the first two signals were introduced, the next most powerful signal was at around 35.5 days, with an analytic false alarm probability of 0.156. Through 104 trials, the false alarm probability was found to be 0.44%, low enough for it to be included as a periodic, planetary signal. With a minimum mass of around 11 Earths, the planet lies at the accepted border between Super-Earths and gaseous, Neptune-like bodies of 10 Earths. After accepting the third signal, a strong peak at 3.6 days became apparent. With a false alarm probability much lower than that of the previously accepted body, it was immediately accepted. With a minimum mass of around 4.5 Earths, it is a small Super-Earth.
As of 2012[update], this system holds the record for the widest range of masses in a single planetary system,[6] and also shows a hierarchy reminiscent of the solar system, with the gas giants at large distances from the star while the smaller bodies are much closer-in.
In 2016, the true mass of Gliese 676 Ab was measured via astrometry.[8] A 2022 study revised this mass estimate, along with measuring the true mass of Gliese 676 Ac.[9] There are two Super-Jupiter planets: "b" with a period of 1051 days (2.9 years) and a mass of 5.79 MJ, and "c" with a period of 13900 days (38.1 years) and a mass of 13.49 MJ, which is at the borderline between planets and brown dwarfs.[9]
Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
d | ≥4.4±0.3 M🜨 | 0.0413±0.0014 | 3.6005±0.0002 | 0.262+0.090 −0.101 |
— | — |
e | ≥8.1±0.7 M🜨 | 0.187±0.007 | 35.39+0.03 −0.04 |
0.125+0.119 −0.087 |
— | — |
b | 5.792+0.469 −0.477 MJ |
1.735+0.056 −0.060 |
1051.4±0.4 | 0.319±0.003 | 48.919+3.312 −2.781° |
— |
c | 13.492+1.046 −1.127 MJ |
9.726+0.629 −0.793 |
13921.4+1238.4 −1518.2 |
0.295+0.033 −0.049 |
33.690+1.362 −1.324° |
— |
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2012 in space
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Selected NEOs |
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Exoplanets |
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Discoveries |
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Comets |
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Space exploration |
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