| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Capricornus |
| Right ascension | 20h 12m 25.87020s[1] |
| Declination | −12° 37′ 02.9967″[1] |
| Apparent magnitude (V) | +5.83[2] |
| Characteristics | |
| Spectral type | F7 V Fe−0.5[3] |
| B−V color index | +0.46[2] |
| Astrometry | |
| Radial velocity (Rv) | +27.1[4] km/s |
| Proper motion (μ) | RA: +192.35[1] mas/yr Dec.: −196.20[1] mas/yr |
| Parallax (π) | 36.10 ± 0.41 mas[1] |
| Distance | 90 ± 1 ly (27.7 ± 0.3 pc) |
| Absolute magnitude (MV) | 3.64±0.02[5] |
| Details[6] | |
| Mass | 1.20+0.01 −0.02 M☉ |
| Surface gravity (log g) | 4.25±0.03 cgs |
| Temperature | 6,411±63 K |
| Metallicity [Fe/H] | −0.25±0.05 dex |
| Rotational velocity (v sin i) | 11[2] km/s |
| Age | 3.04+0.45 −0.51 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Xi2 Capricorni (ξ2 Capricorni) is a yellow-white hued star in the southern constellation of Capricornus. It is dimly visible to the naked eye on a dark night, having an apparent visual magnitude of +5.83.[2] Based upon an annual parallax shift of 36.10 mas as seen from Earth,[1] this system is located 90 light years from the Sun.
This is an F-type main-sequence star with a stellar classification of F7 V Fe−0.5,[3] where the suffix notation indicates the spectrum displays a mild underabundance of iron. It is around three billion years old with 1.2 times the mass of the Sun.[6] Although considered a single star,[8] there is reason to suspect it forms a wide physical pair with the visual magnitude 10.94[9] red dwarf star LP 754–50.[10] They have a projected separation of (28.3±0.3)×103 AU, with LP 754–50 having an estimated 0.55 times the mass of the Sun. If they are gravitationally bound, their orbital period would be around 3.7 million years.[10]
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Теория вероятностей 6.
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References
- ^ 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.
- ^ a b c d Mizusawa, Trisha F.; et al. (November 2012), "Exploring the Effects of Stellar Rotation and Wind Clearing: Debris Disks around F Stars", The Astronomical Journal, 144 (5): 16, arXiv:1208.6248, Bibcode:2012AJ....144..135M, doi:10.1088/0004-6256/144/5/135, S2CID 41406330, 135.
- ^ a b 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: 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
- ^ Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14,000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
- ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
- ^ a b Ramírez, I.; et al. (September 2012), "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets", The Astrophysical Journal, 756 (1): 46, arXiv:1207.0499, Bibcode:2012ApJ...756...46R, doi:10.1088/0004-637X/756/1/46, S2CID 119199829.
- ^ "ksi Cap". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-08-31.
- ^ 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.
- ^ "LP 754-50". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-08-31.
- ^ a b Caballero, J. A. (November 2009), "Reaching the boundary between stellar kinematic groups and very wide binaries. The Washington double stars with the widest angular separations", Astronomy and Astrophysics, 507 (1): 251–259, arXiv:0908.2761, Bibcode:2009A&A...507..251C, doi:10.1051/0004-6361/200912596, S2CID 118194112.
This page was last edited on 14 May 2023, at 13:12