HD 60803

HD 60803
Observation data
Epoch J2000      Equinox J2000
Constellation Canis Minor
Right ascension 07h 36m 34.70576s[1]
Declination 05° 51′ 43.8228″[1]
Apparent magnitude (V) 5.904[2]
Characteristics
Spectral type G0V + G1V[3]
U−B color index 1.351[2]
Astrometry
Radial velocity (Rv)+4.60±0.06[4] km/s
Proper motion (μ) RA: −109.760[1] mas/yr
Dec.: +27.392[1] mas/yr
Parallax (π)24.1025 ± 0.0542 mas[1]
Distance135.3 ± 0.3 ly
(41.49 ± 0.09 pc)
Absolute magnitude (MV)2.93[5]
Orbit[6]
Period (P)26.1889±0.0006 d
Semi-major axis (a)≥16.61±0.04 Gm[3]
Eccentricity (e)0.2187±0.0017
Periastron epoch (T)49644.88±0.03 MJD
Argument of periastron (ω)
(secondary)		113.6±0.5°
Semi-amplitude (K1)
(primary)		47.26±0.10 km/s
Semi-amplitude (K2)
(secondary)		48.16±0.12 km/s
Details
A
Mass1.18±0.08[7] M☉
Radius1.64±0.23[7] R☉
Luminosity6.416±0.020[1] L☉
Surface gravity (log g)4.08±0.12[7] cgs
Temperature6,055±70[7] K
Metallicity [Fe/H]−0.04±0.02[2] dex
Rotational velocity (v sin i)2.6±0.6[3] km/s
Age5.5±0.5[7] Gyr
B
Mass1.15±0.06[7] M☉
Radius1.51±0.16[7] R☉
Surface gravity (log g)4.14±0.09[7] cgs
Temperature6069±70[7] K
Rotational velocity (v sin i)0.9±1.0[3] km/s
Other designations
BD+06°1729, HD 60803, HIP 37031, HR 2918, SAO 115693[8]
Database references
SIMBADdata

HD 60803 is a binary star system in the equatorial constellation of Canis Minor, located less than a degree to the northwest of the prominent star Procyon.[3] It has a yellow hue and is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.904.[2] The distance to this system is 135 light years as determined using parallax measurements,[1] and is drifting further away with a radial velocity of +4.6 km/s.[4]

The binary nature of this star system was first noted by O. C. Wilson and A. Skumanich in 1964.[3] It is a double-lined[9] spectroscopic binary with an orbital period of 26.2 days and an eccentricity of 0.22.[6] Both components are similar, G-type main-sequence stars; the primary has a stellar classification of G0V while the secondary has a class of G1V.[3] The masses are similar to each other, and are 28–31% greater than the mass of the Sun.[9] They have low rotation rates which may be quasi-synchronized with their orbital period.[3]

References

  1. ^ a b c d e f g Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d Netopil, Martin (August 2017), "Metallicity calibrations for dwarf stars and giants in the Geneva photometric system", Monthly Notices of the Royal Astronomical Society, 469 (3): 3042–3055, arXiv:1705.00883, Bibcode:2017MNRAS.469.3042N, doi:10.1093/mnras/stx1077.
  3. ^ a b c d e f g h Griffin, R. F. (August 1997), "Spectroscopic binary orbits from photoelectric radial velocities. Paper 135: HR 2918", The Observatory, 117: 208–213, Bibcode:1997Obs...117..208G.
  4. ^ a b Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  5. ^ 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.
  6. ^ a b Kozłowski, S. K.; et al. (July 2016), "Spectroscopic Survey of Eclipsing Binaries with a Low-cost Echelle Spectrograph: Scientific Commissioning", Publications of the Astronomical Society of the Pacific, 128 (965): 074201, arXiv:1602.01238, Bibcode:2016PASP..128g4201K, doi:10.1088/1538-3873/128/965/074201, S2CID 118633671.
  7. ^ a b c d e f g h i Ryabchikova, T.; Zvyagintsev, S.; Tkachenko, A.; Tsymbal, V.; Pakhomov, Yu; Semenko, E. (2022). "Fundamental parameters and abundance analysis of the components in the SB2 system HD 60803". Monthly Notices of the Royal Astronomical Society. 509: 202–211. arXiv:2110.02637. doi:10.1093/mnras/stab2891.
  8. ^ "HD 60803". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-13.
  9. ^ a b Tokovinin, Andrei (2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 87, arXiv:1401.6827, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, S2CID 56066740.