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61 Leonis

Today, 61 Leonis is a topic that generates great interest and debate in society. From its origins to its current impact, 61 Leonis has been the object of study and reflection by experts and professionals in different fields. Throughout history, 61 Leonis has played a fundamental role in the evolution of humanity, influencing the way we live, work and relate. In this article, we will explore the different aspects of 61 Leonis and its importance in today's world, analyzing its effects and possible implications for the future.

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This article is about p2 Leonis. For other stars with this Bayer designation, see p Leonis.
61 Leonis
Observation data
Epoch J2000      Equinox J2000
Constellation Leo[1]
Right ascension 11h 01m 49.67462s[2]
Declination −02° 29′ 04.5007″[2]
Apparent magnitude (V) 4.73[1]
Characteristics
Evolutionary stage AGB[3]
Spectral type M0 III[4]
B−V color index +1.593±0.059[1]
Variable type suspected[5]
Astrometry
Radial velocity (Rv)−12.7±0.3[6] km/s
Proper motion (μ) RA: +9.76[2] mas/yr
Dec.: −35.56[2] mas/yr
Parallax (π)5.58±0.24 mas[2]
Distance580 ± 30 ly
(179 ± 8 pc)
Absolute magnitude (MV)−1.53[1]
Details
Radius74.5[7] R☉
Luminosity1,377.86[1] L☉
Surface gravity (log g)1.25±0.23[8] cgs
Temperature3,864±30[8] K
Metallicity 0.07±0.07[8] dex
Other designations
p2 Leo, 61 Leo, NSV 5059, BD−01°2471, FK5 2879, HD 95578, HIP 53907, HR 4299, SAO 137947[9]
Database references
SIMBADdata

61 Leonis is a possible binary star[10] system in the zodiac constellation of Leo. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.73.[1] The star is moving closer to the Sun with a heliocentric radial velocity of −12.7 km/s.[6] It is located roughly 580 light-years from the Sun, as determined from its annual parallax shift of 5.58 mas.[2]

This is an evolved red giant star with a stellar classification of M0 III[4] that Eggen (1992) listed as being on the asymptotic giant branch (AGB).[3] It is a marginal barium star, showing an enhanced abundance of s-process elements in its outer atmosphere. This material may have been acquired during a previous mass transfer from a now white dwarf companion, or self-enriched by a dredge-up during the AGB process.[11] The measured angular diameter after correctly for limb darkening is 3.87±0.04 mas,[12] which, at the estimated distance of this system yields a physical size of about 74.5 times the radius of the Sun.[7]

61 Leonis is a suspected variable star with apparent magnitude changing between 4.69 and 4.79.[5] The variability was reported in a 1966 photometric survey, but has not been confirmed by more recent photometry.[13]

References

  1. ^ a b c d e f 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.
  2. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  3. ^ a b Eggen, O. J. (1992), "Asymptotic giant branch stars near the sun", The Astronomical Journal, 104: 275, Bibcode:1992AJ....104..275E, doi:10.1086/116239.
  4. ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373
  5. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  6. ^ a b de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  7. ^ a b Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
  8. ^ a b c Prugniel, Ph.; et al. (2011), "The atmospheric parameters and spectral interpolator for the MILES stars", Astronomy & Astrophysics, 531: A165, arXiv:1104.4952, Bibcode:2011A&A...531A.165P, doi:10.1051/0004-6361/201116769, S2CID 54940439
  9. ^ "61 Leo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-03-01.
  10. ^ 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.
  11. ^ Gomez, A. E.; et al. (1997), "Absolute magnitudes and kinematics of barium stars", Astronomy and Astrophysics, 319: 881, Bibcode:1997A&A...319..881G.
  12. ^ Richichi, A.; et al. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics, 431 (2): 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039
  13. ^ A. W. J. Cousins (1966). "Fabry photometry of bright southern stars". Royal Greenwich Observatory Bulletins. 122: 59. Bibcode:1966RGOB..122...59C.
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