89 Leonis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Leo
Right ascension 11h 34m 21.94862s[1]
Declination +03° 03′ 36.5931″[1]
Apparent magnitude (V) 5.70[2]
Characteristics
Spectral type F5.5V[3]
B−V color index 0.480±0.005[4]
Astrometry
Radial velocity (Rv)+4.775±0.0006[5] km/s
Proper motion (μ) RA: −183.582[1] mas/yr
Dec.: −102.903[1] mas/yr
Parallax (π)36.9527 ± 0.0817 mas[1]
Distance88.3 ± 0.2 ly
(27.06 ± 0.06 pc)
Absolute magnitude (MV)3.53[2]
Details
Mass1.29[2] M☉
Radius1.38±0.04[1] R☉
Luminosity2.990+0.009
−0.010[1] L☉
Surface gravity (log g)4.22[3] cgs
Temperature6,461+93
−90[1] K
Metallicity [Fe/H]−0.04[3] dex
Rotational velocity (v sin i)15.1[2] km/s
Age1.13[2] Gyr
Other designations
89 Leonis, BD+03°2521, FK5 2924, GJ 9367, HD 100563, HIP 56445, HR 4455, SAO 118929[6]
Database references
SIMBADdata

89 Leonis is a single[7] star in the equatorial constellation of Leo, the lion. It has a yellow-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 5.70.[2] Based upon parallax measurements, it is located at a distance of 88 light years from the Sun. The star has a high proper motion[8] and is moving further away with a radial velocity of +4.8 km/s.[5] It is a candidate member of the TW Hydrae stellar kinematic group.[8]

This is an F-type main-sequence star with a stellar classification of F5.5V.[3] It is an estimated 1.13[2] billion years old and is spinning with a rotation period of 7.73 days.[9] It shows evidence of a short-term activity cycle lasting 222.5±3.3 days.[9] The star has 1.3[2] times the mass of the Sun and 1.4[1] times the Sun's radius. It is radiating three[1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,461 K.[1]

References

  1. ^ a b c d e f g h i j k Brown, 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 at VizieR.
  2. ^ a b c d e f g h Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal, 153 (1): 19, arXiv:1611.02897, Bibcode:2017AJ....153...21L, doi:10.3847/1538-3881/153/1/21, S2CID 119511744, 21.
  3. ^ a b c d Gray, R. O.; et al. (2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  4. ^ 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.
  5. ^ a b Soubiran, C.; et al. (2018), "Gaia Data Release 2. The catalogue of radial velocity standard stars", Astronomy and Astrophysics, 616: A7, arXiv:1804.09370, Bibcode:2018A&A...616A...7S, doi:10.1051/0004-6361/201832795, S2CID 52952408.
  6. ^ "89 Leo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-10-05.
  7. ^ 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.
  8. ^ a b Nakajima, Tadashi; Morino, Jun-Ichi (2012), "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun", The Astronomical Journal, 143 (1): 2, Bibcode:2012AJ....143....2N, doi:10.1088/0004-6256/143/1/2.
  9. ^ a b Mittag, M.; et al. (January 2019), "Discovery of short-term activity cycles in F-type stars", Astronomy & Astrophysics, 621: 7, Bibcode:2019A&A...621A.136M, doi:10.1051/0004-6361/201834319, A136.0((citation)): CS1 maint: postscript (link)
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