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54 Leonis

From Wikipedia, the free encyclopedia
Star in the constellation Leo
54 Leonis
Observation data
EpochJ2000.0      Equinox
ConstellationLeo
54 Leo A
Right ascension10h 55m 36.80266s[1]
Declination+24° 44′ 59.0440″[1]
Apparent magnitude (V)4.477[2]
54 Leo B
Right ascension10h 55m 37.24836s[3]
Declination+24° 44′ 56.5478″[3]
Apparent magnitude (V)6.29[4]
Characteristics
54 Leo A
Spectral typeA0 V[5]
B−Vcolor index+0.001[5]
54 Leo B
Spectral typeA2 Vn[5]
B−Vcolor index+0.07[4]
Astrometry
54 Leo A
Radial velocity (Rv)−0.49±0.98[6] km/s
Proper motion (μ)RA: −78.057[1]mas/yr
Dec.: −16.520[1]mas/yr
Parallax (π)9.8275±0.3537 mas[1]
Distance330 ± 10 ly
(102 ± 4 pc)
Absolute magnitude (MV)–0.29[7]
54 Leo B
Radial velocity (Rv)1.30±0.92[6] km/s
Proper motion (μ)RA: −75.374[3] mas/yr
Dec.: −18.595[3] mas/yr
Parallax (π)10.1748 ± 0.0569 mas[3]
Distance321 ± 2 ly
(98.3 ± 0.5 pc)
Details
54 Leo A
Mass2.4+0.44
−0.36
[8] M
Radius2.88[9] R
Surface gravity (log g)3.5±0.25[8] cgs
Temperature9000±500[8] K
Rotational velocity (v sin i)185[10] km/s
Age411+137
−168
[8] Myr
54 Leo B
Radius2.59[9] R
Rotational velocity (v sin i)250±20[9] km/s
Other designations
54 Leo, BD+25 2314, CCDM J10556+2445, HIP 53417, Struve 1487[11]
54 Leo A: HD 94601, HR 4259, SAO 81583
54 Leo B: HD 94602, HR 4260, SAO 81584
Database references
SIMBADdata

54 Leonis is abinary star[12] system in thezodiacconstellation ofLeo, located around 321[3] light years from the Sun. It is visible to the naked eye as a faint, white-hued star with a combinedapparent visual magnitude of 4.30.[13] As of 2017, the pair had anangular separation of6.60 along aposition angle of 113°.[14] They have a physical separation of around 533 AU (79,700 Gm).[9]

The magnitude 4.477[2] primary, designated component A, is anA-type main-sequence star with astellar classification of A0 V,[5] which indicates it is generating energy throughhydrogen fusion at itscore. It has a high rate of spin, showing aprojected rotational velocity of 185 km/s. This is giving the star anoblate shape with anequatorial bulge that is an estimated 8% larger than the polar radius.[10] The star is roughly 411[8] million years old with 2.4[8] times themass of the Sun and about 2.88[9] times theSun's radius.

The fainter magnitude 6.29[4] secondary, component B, is a smaller A-type main-sequence star with a class of A2 Vn.[5] The 'n' suffix indicates wide "nebulous"lines due to rapid rotation. It is spinning with an even higher projected rotational velocity of 250[9] km/s. The star has about 2.59[9] times the Sun's radius.

Asteroid729 Watsoniaocculted HIP 53417 on March 3, 2013 at 01:48.[15]

References

[edit]
  1. ^abcdeBrown, A. G. A.; et al. (Gaia collaboration) (August 2018)."Gaia Data Release 2: Summary of the contents and survey properties".Astronomy & Astrophysics.616. A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source atVizieR.
  2. ^abHøg, E.; et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars",Astronomy and Astrophysics,355: L27,Bibcode:2000A&A...355L..27H,doi:10.1888/0333750888/2862.
  3. ^abcdefBrown, A. G. A.; et al. (Gaia collaboration) (August 2018)."Gaia Data Release 2: Summary of the contents and survey properties".Astronomy & Astrophysics.616. A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source atVizieR.
  4. ^abcFabricius, C.; et al. (2002), "The Tycho double star catalogue",Astronomy and Astrophysics,384:180–189,Bibcode:2002A&A...384..180F,doi:10.1051/0004-6361:20011822
  5. ^abcdeCowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications",Astronomical Journal,74:375–406,Bibcode:1969AJ.....74..375C,doi:10.1086/110819.
  6. ^abBecker, Juliette C.; et al. (April 2015), "Extracting Radial Velocities of A- and B-type Stars from Echelle Spectrograph Calibration Spectra",The Astrophysical Journal Supplement Series,217 (2): 13,arXiv:1503.03874,Bibcode:2015ApJS..217...29B,doi:10.1088/0067-0049/217/2/29,S2CID 33968873, 29.
  7. ^Pizzolato, N.; Maggio, A.; Sciortino, S. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases",Astronomy and Astrophysics,361:614–628,Bibcode:2000A&A...361..614P
  8. ^abcdefGullikson, Kevin; et al. (2016), "The Close Companion Mass-ratio Distribution of Intermediate-mass Stars",The Astronomical Journal,152 (2): 40,arXiv:1604.06456,Bibcode:2016AJ....152...40G,doi:10.3847/0004-6256/152/2/40,S2CID 119179065.
  9. ^abcdefgHowe, K. S.; Clarke, C. J. (January 2009), "An analysis of v sin (i) correlations in early-type binaries",Monthly Notices of the Royal Astronomical Society,392 (1):448–454,Bibcode:2009MNRAS.392..448H,doi:10.1111/j.1365-2966.2008.14073.x
  10. ^abBelle, G. T. (2012), "Interferometric observations of rapidly rotating stars",The Astronomy and Astrophysics Review,20 (1): 51,arXiv:1204.2572,Bibcode:2012A&ARv..20...51V,doi:10.1007/s00159-012-0051-2,S2CID 119273474.
  11. ^"54 Leo".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2019-02-05.
  12. ^Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems",Monthly Notices of the Royal Astronomical Society,389 (2):869–879,arXiv:0806.2878,Bibcode:2008MNRAS.389..869E,doi:10.1111/j.1365-2966.2008.13596.x,S2CID 14878976.
  13. ^Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation",Astronomy Letters,38 (5): 331,arXiv:1108.4971,Bibcode:2012AstL...38..331A,doi:10.1134/S1063773712050015,S2CID 119257644.
  14. ^Mason, Brian D.; et al. (December 2001), "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog",The Astronomical Journal,122 (6), U. S. Naval Observatory, Washington D.C.:3466–3471,Bibcode:2001AJ....122.3466M,doi:10.1086/323920.
  15. ^Pier Paolo Ricci (29 November 2012).Almanacco astronomico 2013 Astronomical almanac 2013. Lulu.com. pp. 322–.ISBN 978-1-291-21157-3.
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