Back Praecipua Afrikaans Praecipua AST Praecipua (estel) Catalan Praecipua Czech 46 Leonis Minoris German Praecipua Spanish 46 Leonis Minoris French 46 Leonis Minoris ID 46 Leonis Minoris Italian こじし座46番星 Japanese
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo Minor |
| Right ascension | 10h 53m 18.70487s[1] |
| Declination | +34° 12′ 53.5375″[1] |
| Apparent magnitude (V) | 3.83[2] (3.79–3.84[3]) |
| Characteristics | |
| Evolutionary stage | red clump[4] |
| Spectral type | K0+ III-IV[5] |
| Variable type | suspected[3] |
| Astrometry | |
| Proper motion (μ) | RA: +92.02[1] mas/yr Dec.: −285.82[1] mas/yr |
| Parallax (π) | 34.38 ± 0.21 mas[1] |
| Distance | 94.9 ± 0.6 ly (29.1 ± 0.2 pc) |
| Absolute magnitude (MV) | +1.45[6] |
| Details | |
| Mass | 1.69[7] M☉ |
| Radius | 8.22 ± 0.22[2] R☉ |
| Luminosity | 34 ± 2[2] L☉ |
| Surface gravity (log g) | 2.96[2] cgs |
| Temperature | 4,670[2] K |
| Metallicity [Fe/H] | −0.20[8] dex |
| Rotational velocity (v sin i) | 1.81[9] km/s |
| Age | 6.76[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
46 Leonis Minoris (abbreviated 46 LMi), also named Praecipua /prɪˈsɪpjʊə/,[10] is the brightest star in the constellation of Leo Minor. It is of spectral class K0+III-IV and of magnitude 3.83. It is a red clump giant.[4] Based upon parallax measurements, its distance from the Sun is approximately 95 light-years. It is a suspected variable with an amplitude of about 0.05 magnitudes.[3]
- ^ a b c d e Cite error: The named reference
aaa474_2_653was invoked but never defined (see the help page). - ^ a b c d e Cite error: The named reference
aaa526_A100was invoked but never defined (see the help page). - ^ a b c 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.
- ^ a b c Soubiran, C.; Bienaymé, O.; Mishenina, T. V.; Kovtyukh, V. V. (2008). "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants". Astronomy and Astrophysics. 480 (1): 91–101. arXiv:0712.1370. Bibcode:2008A&A...480...91S. doi:10.1051/0004-6361:20078788. S2CID 16602121.
- ^ 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.
- ^ Mullan, D. J.; MacDonald, J. (2003). "Onset of Mass Loss in Red Giants: Association with an Evolutionary Event". The Astrophysical Journal. 591 (2): 1203. Bibcode:2003ApJ...591.1203M. doi:10.1086/375446.
- ^ Lyubimkov, L. S.; Poklad, D. B. (2014). "Determining the effective temperatures of G- and K-type giants and supergiants based on observed photometric indices". Kinematics and Physics of Celestial Bodies. 30 (5): 244. arXiv:1412.6950. Bibcode:2014KPCB...30..244L. doi:10.3103/S0884591314050055. S2CID 118618820.
- ^ Wittenmyer, Robert A.; Gao, Dongyang; Hu, Shao Ming; Villaver, Eva; Endl, Michael; Wright, Duncan (2015). "The Weihai Observatory Search for Close-in Planets Orbiting Giant Stars". Publications of the Astronomical Society of the Pacific. 127 (956): 1021. arXiv:1507.06051. Bibcode:2015PASP..127.1021W. doi:10.1086/683258. S2CID 117305333.
- ^ Hekker, S.; Meléndez, J. (2007). "Precise radial velocities of giant stars. III. Spectroscopic stellar parameters". Astronomy and Astrophysics. 475 (3): 1003. arXiv:0709.1145. Bibcode:2007A&A...475.1003H. doi:10.1051/0004-6361:20078233. S2CID 10436552.
- ^ "Naming Stars". IAU.org. Retrieved 16 December 2017.
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