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]

  1. ^ a b c d e f g Cite error: The named reference GaiaDR2 was invoked but never defined (see the help page).
  2. ^ a b c d Cite error: The named reference Netopil2017 was invoked but never defined (see the help page).
  3. ^ a b c d e f g h Cite error: The named reference Griffin1997 was invoked but never defined (see the help page).
  4. ^ a b Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  5. ^ Cite error: The named reference Holmberg2009 was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference Kozłowski2016 was invoked but never defined (see the help page).
  7. ^ a b c d e f g h i Cite error: The named reference Ryabchikova2021 was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  9. ^ a b Cite error: The named reference tokovinin2014 was invoked but never defined (see the help page).