HD 60803
Star in the constellation Canis Minor
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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.[4] 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.[3] The distance to this system is 135 light years as determined using parallax measurements,[2] and is drifting further away with a radial velocity of +4.6 km/s.[1]
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Canis Minor[1] |
| Right ascension | 07h 36m 34.70576s[2] |
| Declination | 05° 51′ 43.8228″[2] |
| Apparent magnitude (V) | 5.904[3] |
| Characteristics | |
| Spectral type | G0V + G1V[4] |
| U−B color index | 1.351[3] |
| Astrometry | |
| Radial velocity (Rv) | +4.60±0.06[1] km/s |
| Proper motion (μ) | RA: −109.760[2] mas/yr Dec.: +27.392[2] mas/yr |
| Parallax (π) | 24.1025±0.0542 mas[2] |
| Distance | 135.3 ± 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[4] |
| 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 | |
| Mass | 1.18±0.08[7] M☉ |
| Radius | 1.64±0.23[7] R☉ |
| Luminosity | 6.416±0.020[2] L☉ |
| Surface gravity (log g) | 4.08±0.12[7] cgs |
| Temperature | 6,055±70[7] K |
| Metallicity [Fe/H] | −0.04±0.02[3] dex |
| Rotational velocity (v sin i) | 2.6±0.6[4] km/s |
| Age | 5.5±0.5[7] Gyr |
| B | |
| Mass | 1.15±0.06[7] M☉ |
| Radius | 1.51±0.16[7] R☉ |
| Surface gravity (log g) | 4.14±0.09[7] cgs |
| Temperature | 6069±70[7] K |
| Rotational velocity (v sin i) | 0.9±1.0[4] km/s |
| Other designations | |
| BD+06°1729, HD 60803, HIP 37031, HR 2918, SAO 115693[8] | |
| Database references | |
| SIMBAD | data |
The binary nature of this star system was first noted by O. C. Wilson and A. Skumanich in 1964.[4] 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.[4] 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.[4]