Astronomy:Xi2 Capricorni
| Observation data 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[1] mas |
| 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 astronomical unit|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]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 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, doi:10.1088/0004-6256/144/5/135, 135, Bibcode: 2012AJ....144..135M.
- ↑ 3.0 3.1 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, doi:10.1086/504637, Bibcode: 2006AJ....132..161G.
- ↑ 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, doi:10.1051/0004-6361:20035959, Bibcode: 2004A&A...418..989N.
- ↑ 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, doi:10.1051/0004-6361/200811191, Bibcode: 2009A&A...501..941H.
- ↑ 6.0 6.1 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, doi:10.1088/0004-637X/756/1/46, Bibcode: 2012ApJ...756...46R.
- ↑ "ksi Cap". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=ksi+Cap.
- ↑ 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.
- ↑ "LP 754-50". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=LP+754-50.
- ↑ 10.0 10.1 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, doi:10.1051/0004-6361/200912596, Bibcode: 2009A&A...507..251C.
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