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] |
| 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[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 | |
| Mass | 1.18±0.08[7] M☉ |
| Radius | 1.64±0.23[7] R☉ |
| Luminosity | 6.416±0.020[1] L☉ |
| Surface gravity (log g) | 4.08±0.12[7] cgs |
| Temperature | 6,055±70[7] K |
| Metallicity [Fe/H] | −0.04±0.02[2] dex |
| Rotational velocity (v sin i) | 2.6±0.6[3] km/s |
| 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[3] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
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
[edit]- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ "HD 60803". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-13.
- ^ 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.
