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{{Short description|Star in the constellation Leo}} |
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{{Starbox begin |
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| name=φ Leonis |
| name=φ Leonis |
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{{Starbox catalog |
{{Starbox catalog |
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| names = [[Bayer designation|φ |
| names = [[Bayer designation|φ Leo]], [[Flamsteed designation|74 Leo]], [[Bonner Durchmusterung|BD]]−02°3315, [[FK5]] 1292, [[Henry Draper Catalogue|HD]] 98058, [[Hipparcos catalogue|HIP]] 55084, [[Harvard Revised catalogue|HR]] 4368, [[Smithsonian Astrophysical Observatory catalogue|SAO]] 138102<ref name=SIMBAD/> |
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}} |
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{{Starbox reference |
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| Simbad = phi+Leo |
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}} |
}} |
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{{Starbox end}} |
{{Starbox end}} |
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'''Phi Leonis''' ('''φ Leo''') is a [[star]] in the [[constellation]] [[Leo (constellation)|Leo]]. It is bright enough to be seen with the naked eye, having an [[apparent visual magnitude]] of 4.46.<ref name=Mermilliod1986/> Based upon [[stellar parallax|parallax]] measurements,<ref name=vanLeeuwen2007/> the distance to Phi Leo is around 184 [[light year]]s. |
'''Phi Leonis''' ('''φ Leo''') is a single<ref name=Hutter/> [[star]] in the [[constellation]] [[Leo (constellation)|Leo]]. It is bright enough to be seen with the naked eye, having an [[apparent visual magnitude]] of 4.46.<ref name=Mermilliod1986/> Based upon [[stellar parallax|parallax]] measurements,<ref name=vanLeeuwen2007/> the distance to Phi Leo is around 184 [[light year]]s. |
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The spectrum of this star fits a [[stellar classification]] of A7IVn,<ref name=Royer2007/> which suggests it is an [[A-type star|A-type]] [[subgiant star]] that has left the [[main sequence]] and is [[stellar evolution|evolving]] into a [[giant star]]. It is being viewed with the plane of the star's [[equator]] lying close the line of sight from the Earth,<ref name=Eiroa/> and shows a high rotation rate with a [[projected rotational velocity]] of 254 km/s.<ref name=Royer2007/> This rapid spin is giving the star an [[Oblate spheroid|oblate shape]] with an [[equatorial bulge]] that is 29% larger than the polar radius.<ref name=aar20_1_51/> |
The spectrum of this star fits a [[stellar classification]] of A7IVn,<ref name=Royer2007/> which suggests it is an [[A-type star|A-type]] [[subgiant star]] that has left the [[main sequence]] and is [[stellar evolution|evolving]] into a [[giant star]]. It is being viewed with the plane of the star's [[equator]] lying close the line of sight from the Earth,<ref name=Eiroa/> and shows a high rotation rate with a [[projected rotational velocity]] of 254 km/s.<ref name=Royer2007/> This rapid spin is giving the star an [[Oblate spheroid|oblate shape]] with an [[equatorial bulge]] that is 29% larger than the polar radius.<ref name=aar20_1_51/> |
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Phi Leonis has been mentioned as a [[shell star]]—indicating that there is a circumstellar disk of gas around the star's equator—and may display a slight [[variable star|variability]].<ref name=aaa354_157/> Sporadic variation of the spectra on the time scale of minutes up to months in duration suggests that solid, cometary bodies are in orbit around the star, with objects approaching close enough for [[refractory]] materials to [[Sublimation (phase transition)|sublimate]].<ref name=Eiroa/> |
Phi Leonis has been mentioned as a [[shell star]]—indicating that there is a circumstellar disk of gas around the star's equator—and may display a slight [[variable star|variability]].<ref name=aaa354_157/> Sporadic variation of the spectra on the time scale of minutes up to months in duration suggests that solid, cometary bodies are in orbit around the star, with objects approaching close enough for [[refractory]] materials to [[Sublimation (phase transition)|sublimate]].<ref name=Eiroa/> Most [[exocomet]] hosts do have a [[Circumstellar disc|circumstellar disk]], which can act as an exocomet reservoir. Cold dust around Phi Leonis was not detected, and the star is not associated with a warm debris disk.<ref>{{Cite journal|last1=Cataldi|first1=Gianni|last2=Moór|first2=Attila|last3=Ohashi|first3=Nagayoshi|last4=Eiroa|first4=Carlos|last5=Grady|first5=Carol|last6=Rebollido|first6=Isabel|date=2019-02-22|title=No Detection of Cold Dust around the Potential Exocomet Host ϕ Leo|journal=Research Notes of the AAS|language=en|volume=3|issue=2|pages=39|doi=10.3847/2515-5172/ab082b|bibcode=2019RNAAS...3...39C |s2cid=127680980 |issn=2515-5172 |doi-access=free }}</ref> |
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==References== |
==References== |
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| Line 53: | Line 57: | ||
| volume=474 | issue=2 | pages=653–664 | date=2007 |
| volume=474 | issue=2 | pages=653–664 | date=2007 |
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| arxiv=0708.1752 | bibcode=2007A&A...474..653V |
| arxiv=0708.1752 | bibcode=2007A&A...474..653V |
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| doi=10.1051/0004-6361:20078357 | postscript=. }}</ref> |
| doi=10.1051/0004-6361:20078357 | s2cid=18759600 | postscript=. }}</ref> |
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<ref name=Royer2007>{{citation |
<ref name=Royer2007>{{citation |
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| Line 62: | Line 66: | ||
| volume=463 | issue=2 | pages=671–682 | date=February 2007 |
| volume=463 | issue=2 | pages=671–682 | date=February 2007 |
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| doi=10.1051/0004-6361:20065224 | bibcode=2007A&A...463..671R |
| doi=10.1051/0004-6361:20065224 | bibcode=2007A&A...463..671R |
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| arxiv=astro-ph/0610785 | postscript=. }}</ref> |
| arxiv=astro-ph/0610785 | s2cid=18475298 | postscript=. }}</ref> |
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<ref name=Wielen1999>{{citation |
<ref name=Wielen1999>{{citation |
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| title=Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic Fundamental Stars with Direct Solutions |
| title=Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic Fundamental Stars with Direct Solutions |
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| journal=Veroeffentlichungen des Astronomischen Rechen-Instituts Heidelberg |
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| volume=35 |
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| display-authors=1 |
| display-authors=1 |
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| last1=Wielen | first1=R. | last2=Schwan | first2=H. |
| last1=Wielen | first1=R. | last2=Schwan | first2=H. |
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| Line 71: | Line 77: | ||
| last5=Jahreiß | first5=H. | last6=Jährling | first6=R. |
| last5=Jahreiß | first5=H. | last6=Jährling | first6=R. |
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| publisher=Astronomisches Rechen-Institut Heidelberg |
| publisher=Astronomisches Rechen-Institut Heidelberg |
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| issue=35 | date=1999 |
| issue=35 | pages=1 |
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| date=1999 |
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| bibcode=1999VeARI..35....1W | postscript=. }}</ref> |
| bibcode=1999VeARI..35....1W | postscript=. }}</ref> |
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| Line 81: | Line 88: | ||
| volume=804 | issue=2 | pages=146 | year=2015 |
| volume=804 | issue=2 | pages=146 | year=2015 |
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| bibcode=2015ApJ...804..146D | doi=10.1088/0004-637X/804/2/146 |
| bibcode=2015ApJ...804..146D | doi=10.1088/0004-637X/804/2/146 |
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| arxiv=1501.03154 | postscript=. }}</ref> |
| arxiv=1501.03154 | s2cid=33401607 |
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| postscript=. }}</ref> |
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<ref name=aar20_1_51>{{citation |
<ref name=aar20_1_51>{{citation |
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| Line 89: | Line 97: | ||
| volume=20 | issue=1 | page=51 |date=March 2012 |
| volume=20 | issue=1 | page=51 |date=March 2012 |
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| doi=10.1007/s00159-012-0051-2 | bibcode=2012A&ARv..20...51V |
| doi=10.1007/s00159-012-0051-2 | bibcode=2012A&ARv..20...51V |
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| arxiv=1204.2572 | postscript=. }}</ref> |
| arxiv=1204.2572 | s2cid=119273474 |
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| postscript=. }}</ref> |
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<ref name=cadars>{{citation |
<ref name=cadars>{{citation |
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| Line 97: | Line 106: | ||
| title=Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics |
| title=Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics |
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| journal=Astronomy & Astrophysics |
| journal=Astronomy & Astrophysics |
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| volume=367 | pages=521–24 | date=2001 |
| volume=367 | issue=2 | pages=521–24 | date=2001 |
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| bibcode=2001A&A...367..521P | doi=10.1051/0004-6361:20000451 |
| bibcode=2001A&A...367..521P | doi=10.1051/0004-6361:20000451 |
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| arxiv=astro-ph/0012289 | postscript=. }}</ref> |
| arxiv=astro-ph/0012289 | s2cid=425754 | postscript=. }}</ref> |
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<ref name=aaa354_157>{{citation |
<ref name=aaa354_157>{{citation |
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| Line 115: | Line 124: | ||
| volume=427 | issue=1 | pages=343–57 | date=2012 |
| volume=427 | issue=1 | pages=343–57 | date=2012 |
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| bibcode=2012MNRAS.427..343M | arxiv=1208.2037 |
| bibcode=2012MNRAS.427..343M | arxiv=1208.2037 |
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| doi=10.1111/j.1365-2966.2012.21873.x | postscript=. }}</ref> |
| doi=10.1111/j.1365-2966.2012.21873.x | s2cid=118665352 | postscript=. }}</ref> |
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<ref name=Hutter>{{cite journal |
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| title=Surveying the Bright Stars by Optical Interferometry. III. A Magnitude-limited Multiplicity Survey of Classical Be Stars | year=2021 |
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| last1=Hutter | first1=D. J. | last2=Tycner | first2=C. |
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| last3=Zavala | first3=R. T. | last4=Benson | first4=J. A. |
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| last5=Hummel | first5=C. A. | last6=Zirm | first6=H. |
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| journal=The Astrophysical Journal Supplement Series |
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| volume=257 | issue=2 | page=69 |
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| doi=10.3847/1538-4365/ac23cb | arxiv=2109.06839 |
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| bibcode=2021ApJS..257...69H | s2cid=237503492 | doi-access=free |
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}}</ref> |
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<ref name=Mermilliod1986>{{citation |
<ref name=Mermilliod1986>{{citation |
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| last1=Mermilliod | first1=J.-C. |
| last1=Mermilliod | first1=J.-C. |
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| title=Compilation of Eggen's UBV data, transformed to UBV (unpublished) |
| title=Compilation of Eggen's UBV data, transformed to UBV (unpublished) |
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| journal=Catalogue of Eggen's UBV Data |
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| publisher=SIMBAD | date=1986 | bibcode=1986EgUBV........0M | postscript=. }}</ref> |
| publisher=[[SIMBAD]] | date=1986 | bibcode=1986EgUBV........0M | postscript=. }}</ref> |
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<ref name=Eiroa>{{citation |
<ref name=Eiroa>{{citation |
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| Line 137: | Line 158: | ||
| first22=A. | last22=Roberge |
| first22=A. | last22=Roberge |
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| title=Exocomet signatures around the A-shell star Φ Leo? |
| title=Exocomet signatures around the A-shell star Φ Leo? |
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| journal=Astronomy & Astrophysics | volume=L1 | pages=594 | date=September 14, 2016 |
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| publisher=Cornell University | work=arXiv.org |
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| arxiv=1609.04263 | postscript=. |doi = 10.1051/0004-6361/201629514 |bibcode = 2016A&A...594L...1E | s2cid=41231308 | url=http://orbi.ulg.ac.be/bitstream/2268/204875/1/aa29514-16.pdf}}</ref> |
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| date=September 14, 2016 |
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| arxiv=1609.04263 | postscript=. }}</ref> |
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<ref name=SIMBAD>{{ |
<ref name=SIMBAD>{{cite simbad |
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| title=ups Leo |
| title=ups Leo |
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| work=SIMBAD Astronomical Database |
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| publisher=Centre de Données astronomiques de Strasbourg |
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| url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=phi+leo |
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| accessdate=2016-09-29 | postscript=. }}</ref> |
| accessdate=2016-09-29 | postscript=. }}</ref> |
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| Line 152: | Line 169: | ||
{{Stars of Leo|state=collapsed}} |
{{Stars of Leo|state=collapsed}} |
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{{DEFAULTSORT:Phi Leonis}} |
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[[Category:A-type subgiants]] |
[[Category:A-type subgiants]] |
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[[Category:Shell stars]] |
[[Category:Shell stars]] |
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| Line 159: | Line 177: | ||
[[Category:Henry Draper Catalogue objects|098058]] |
[[Category:Henry Draper Catalogue objects|098058]] |
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[[Category:Hipparcos objects|055084]] |
[[Category:Hipparcos objects|055084]] |
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[[Category: |
[[Category:Bright Star Catalogue objects|4368]] |
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[[Category:Durchmusterung objects]] |
[[Category:Durchmusterung objects]] |
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| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Leo |
| Right ascension | 11h16m 39.69960s[1] |
| Declination | −03° 39′ 05.7770″[1] |
| Apparent magnitude (V) | 4.46[2] |
| Characteristics | |
| Spectral type | A7 IVn[3] |
| U−B color index | +0.10[2] |
| B−V color index | +0.22[2] |
| Astrometry | |
| Radial velocity (Rv) | −3.0[4] km/s |
| Proper motion (μ) | RA: −110.37[1] mas/yr Dec.: −37.16[1] mas/yr |
| Parallax (π) | 17.71 ± 0.25 mas[1] |
| Distance | 184 ± 3 ly (56.5 ± 0.8 pc) |
| Absolute magnitude (MV) | 0.56[5] |
| Details | |
| Mass | 1.59[6] M☉ |
| Radius | 2.9[7] R☉ |
| Luminosity | 39[8] L☉ |
| Surface gravity (log g) | 3.56[3] cgs |
| Temperature | 7,680±261[3] K |
| Rotational velocity (v sin i) | 254[3] km/s |
| Age | 432[3] Myr |
| Other designations | |
φ Leo, 74 Leo, BD−02°3315, FK5 1292, HD 98058, HIP 55084, HR 4368, SAO 138102[9] | |
| Database references | |
| SIMBAD | data |
Phi Leonis (φ Leo) is a single[10] star in the constellation Leo. It is bright enough to be seen with the naked eye, having an apparent visual magnitude of 4.46.[2] Based upon parallax measurements,[1] the distance to Phi Leo is around 184 light years.
The spectrum of this star fits a stellar classification of A7IVn,[3] which suggests it is an A-type subgiant star that has left the main sequence and is evolving into a giant star. It is being viewed with the plane of the star's equator lying close the line of sight from the Earth,[11] and shows a high rotation rate with a projected rotational velocity of 254 km/s.[3] This rapid spin is giving the star an oblate shape with an equatorial bulge that is 29% larger than the polar radius.[12]
Phi Leonis has been mentioned as a shell star—indicating that there is a circumstellar disk of gas around the star's equator—and may display a slight variability.[5] Sporadic variation of the spectra on the time scale of minutes up to months in duration suggests that solid, cometary bodies are in orbit around the star, with objects approaching close enough for refractory materials to sublimate.[11] Most exocomet hosts do have a circumstellar disk, which can act as an exocomet reservoir. Cold dust around Phi Leonis was not detected, and the star is not associated with a warm debris disk.[13]
{{cite web}}: CS1 maint: postscript (link)
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