Astronomy:89 Leonis
| Observation data Epoch J2000.0 Equinox (celestial coordinates) | |
|---|---|
| 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[1] mas |
| Distance | 88.3 ± 0.2 ly (27.06 ± 0.06 pc) |
| Absolute magnitude (MV) | 3.53[2] |
| Details | |
| Mass | 1.29[2] M☉ |
| Radius | 1.38±0.04[1] R☉ |
| Luminosity | 2.990+0.009 −0.010[1] L☉ |
| Surface gravity (log g) | 4.22[3] cgs |
| Temperature | 6,461+93 −90[1] K |
| Metallicity [Fe/H] | −0.04[3] dex |
| Rotational velocity (v sin i) | 15.1[2] km/s |
| Age | 1.13[2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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
- ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal 153 (1): 19, doi:10.3847/1538-3881/153/1/21, 21, Bibcode: 2017AJ....153...21L.
- ↑ 3.0 3.1 3.2 3.3 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, doi:10.1086/504637, Bibcode: 2006AJ....132..161G.
- ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 5.0 5.1 Soubiran, C. et al. (2018), "Gaia Data Release 2. The catalogue of radial velocity standard stars", Astronomy and Astrophysics 616: A7, doi:10.1051/0004-6361/201832795, Bibcode: 2018A&A...616A...7S.
- ↑ "89 Leo". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=89+Leo.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 8.0 8.1 Nakajima, Tadashi; Morino, Jun-Ichi (2012), "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun", The Astronomical Journal 143 (1): 2, doi:10.1088/0004-6256/143/1/2, Bibcode: 2012AJ....143....2N.
- ↑ 9.0 9.1 Mittag, M. et al. (January 2019), "Discovery of short-term activity cycles in F-type stars", Astronomy & Astrophysics 621: 7, doi:10.1051/0004-6361/201834319, A136, Bibcode: 2019A&A...621A.136M.0
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