For other stars with this Bayer designation, see
ξ Capricorni.
Xi2 Capricorni
Observation data
Epoch J2000.0 Equinox J2000.0 (ICRS)
|
| Constellation
|
Capricornus
|
| Right ascension
|
20h 12m 25.871s[1]
|
| Declination
|
−12° 37′ 02.99″[1]
|
| Apparent magnitude (V)
|
+5.83[2]
|
| Characteristics
|
| Evolutionary stage
|
main sequence[1]
|
| 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: +193.111 mas/yr[1]
Dec.: −195.662 mas/yr[1] |
| Parallax (π) | 35.4185±0.0351 mas[1] |
| Distance | 92.09 ± 0.09 ly
(28.23 ± 0.03 pc) |
| Absolute magnitude (MV) | 3.64±0.02[5] |
|
|---|
| Details |
|---|
|
|---|
| Mass | 1.23±0.04[1] M☉ |
| Radius | 1.50±0.03[1] R☉ |
| Luminosity | 3.07±0.01[1] L☉ |
| Surface gravity (log g) | 4.151±0.001[1] cgs |
| Temperature | 6,248±1[1] K |
| Metallicity [Fe/H] | −0.25±0.05[6] dex |
| Rotational velocity (v sin i) | 11[2] km/s |
| Age | 3.47±0.53[1] Gyr |
|
|---|
| Other designations |
|---|
| ξ2 Cap, 2 Cap, BD−13°5608, GC 28035, GJ 4139, HD 191862, HIP 99572, HR 7715, SAO 163337, CCDM J20124-1237, WDS J20124-1237A[7] |
| Database references |
|---|
| SIMBAD | data |
Xi2 Capricorni is a yellow-white hued star in the southern constellation of Capricornus. Its name is a Bayer designation that is Latinized from ξ2 Capricorni, and abbreviated Xi2 Cap or ξ2 Cap. This star 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 35.42 mas as seen from Earth,[1] this system is located at a distance of 92 light-years (28 pc) from the Sun. It is drifting further away with a line of sight velocity of +27 km/s.[4]
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 3.5 billion years old and is spinning with a projected rotational velocity of 11 km/s.[2] The star has 1.2 times the mass of the Sun and 1.5 times the Sun's radius. It is radiating three times the luminosity of the Sun from its photosphere at an effective temperature of 6,248 K.[1]
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 28,300±300 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
- ^ a b c d e f g h i j k l m Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875.
Gaia DR3 record for this source at VizieR.
- ^ a b c d e 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 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
- ^ a b 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.
- ^ 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.
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