Rho Capricorni

Rho Capricorni
Location of ρ Capricorni (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Capricornus
Right ascension 20h 28m 51.615s[1]
Declination −17° 48′ 49.26″[1]
Apparent magnitude (V) +4.78[2] (4.97 + 6.88)[3]
Characteristics
Spectral type F2 IV[2] + G1[4]
B−V color index 0.340/0.635[5]
Astrometry
Radial velocity (Rv)+18.4[6] km/s
Proper motion (μ) RA: −16.889 mas/yr[1]
Dec.: −10.579 mas/yr[1]
Parallax (π)33.2297±0.2146 mas[1]
Distance98.2 ± 0.6 ly
(30.1 ± 0.2 pc)
Absolute magnitude (MV)2.52 + 4.56[4]
Orbit[3]
Period (P)278 yr
Semi-major axis (a)1.877″
Eccentricity (e)0.91
Inclination (i)113.3°
Longitude of the node (Ω)162.0°
Periastron epoch (T)1965.0
Argument of periastron (ω)
(secondary)		144.5°
Details[7]
ρ Cap A
Mass1.52±0.04 M☉
Radius1.3[2] R☉
Luminosity9[8] L☉
Surface gravity (log g)4.02±0.03 cgs
Temperature6,911±63 K
Metallicity [Fe/H]−0.20±0.05 dex
Rotational velocity (v sin i)87.7[9] km/s
Age1.74±0.15 Gyr
Other designations
ρ Cap, 11 Cap, BD−18°5689, GJ 791.1, GJ 9696, HD 194943, HIP 101027, HR 7822, SAO 163614, ADS 13887, WDS J20289-1749AB[10]
Database references
SIMBADρ Cap
ρ Cap A
ρ Cap B
ARICNSρ Cap A
ρ Cap B

Rho Capricorni is a binary star[3] system in the constellation Capricornus. Its name is a Bayer designation that is Latinized from ρ Capricorni, and abbreviated Rho Cap or ρ Cap. Sometimes, this star is called by the name Bos, meaning the cow in Latin.[11] In Chinese, 牛宿 (Niú Su), meaning Ox (asterism), refers to an asterism consisting of β Capricorni, α2 Capricorni, ξ2 Capricorni, π Capricorni, ο Capricorni and ρ Capricorni.[12] Consequently, the Chinese name for ρ Capricorni itself is 牛宿六 (Niú Su liù, English: the Sixth Star of Ox.)[13]

This system is visible to the naked eye with a combined apparent visual magnitude of +4.78.[2] The pair orbit each other with a period of 278 years and an eccentricity of 0.91.[3] Based upon an annual parallax shift of 33.23 mas as seen from the Earth,[1] the system is located about 98 light-years (30 pc) distant from the Sun. It is a thin disk population[7] star system that made its closest approach to the Sun about 1.6 million years ago when it came within 12.49 ly (3.830 pc).[14] Based upon its motion through space, this system may be a member of the Ursa Major moving group of stars.[5]

The primary member, component A, is a yellow-white hued, F-type subgiant with an apparent magnitude of 4.97[3] and a stellar classification of F2 IV.[2] This star has 1.5[7] times the mass of the Sun and 1.3 times the Sun's radius. It is radiating 9 times[8] as much luminosity of the Sun from its outer atmosphere at an effective temperature of 6,911 K.[7] The companion, component B, has a visual magnitude of 6.88.[3] The mass ratio is 0.539, meaning the secondary is only 53.9% as massive as the primary.[15]

References

  1. ^ a b c d e 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.
  2. ^ a b c d e Malagnini, M. L.; Morossi, C. (November 1990), "Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars", Astronomy and Astrophysics Supplement Series, 85 (3): 1015–1019, Bibcode:1990A&AS...85.1015M.
  3. ^ a b c d e f Sixth Catalog of Orbits of Visual Binary Stars, United States Naval Observatory, archived from the original on 2005-04-24, retrieved 2017-05-12
  4. ^ a b Cvetkovic, Z.; Ninkovic, S. (June 2010), "On the Component Masses of Visual Binaries", Serbian Astronomical Journal, 180 (180): 71–80, Bibcode:2010SerAJ.180...71C, doi:10.2298/SAJ1080071C.
  5. ^ a b King, Jeremy R.; et al. (April 2003), "Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group", The Astronomical Journal, 125 (4): 1980–2017, Bibcode:2003AJ....125.1980K, doi:10.1086/368241.
  6. ^ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
  7. ^ a b c d 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.
  8. ^ a b McDonald, I.; et al. (2012), "Fundamental parameters and infrared excesses of Hipparcos stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–357, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
  9. ^ Schröder, C.; et al. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo", Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377
  10. ^ "rho Cap", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-05-12.
  11. ^ "Bos", constellationsofwords.com, retrieved 2017-05-12.
  12. ^ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
  13. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 13 日 Archived 2011-05-22 at the Wayback Machine
  14. ^ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv:1412.3648, Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, S2CID 59039482, A35.
  15. ^ Makarov, Valeri V.; Fabricius, Claus (2021), "Astrometric Mass Ratios of 248 Long-period Binary Stars Resolved in Hipparcos and Gaia EDR3", The Astronomical Journal, 162 (6): 260, arXiv:2109.11951, Bibcode:2021AJ....162..260M, doi:10.3847/1538-3881/ac2ee0, S2CID 237635330.
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