Astronomy:Gamma Canis Minoris
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Canis Minor |
| Right ascension | 07h 28m 09.794s[1] |
| Declination | +08° 55′ 31.89″[1] |
| Apparent magnitude (V) | +4.33[2] (4.46 + 6.66)[2] |
| Characteristics | |
| Spectral type | K3 III Fe-0.5[3] (K4 III + K1: III)[2] |
| U−B color index | +1.53[4] |
| B−V color index | +1.43[4] |
| Astrometry | |
| Radial velocity (Rv) | 46.8±0.3[5] km/s |
| Proper motion (μ) | RA: −62.112[1] mas/yr Dec.: −11.141[1] mas/yr |
| Parallax (π) | 3.134 ± 0.1714[1] mas |
| Distance | 1,040 ± 60 ly (320 ± 20 pc) |
| Absolute magnitude (MV) | −0.5±0.1[2] |
| Absolute magnitude (MV) | 1.7±0.2[2] |
| Orbit[2] | |
| Period (P) | 389.310±0.012d |
| Semi-major axis (a) | 17 mas |
| Eccentricity (e) | 0.25856±0.00039 |
| Inclination (i) | 66° |
| Periastron epoch (T) | 2449849.172±0.089 HJD |
| Argument of periastron (ω) (secondary) | 142.079±0.090° |
| Semi-amplitude (K1) (primary) | 21.243±0.010 km/s |
| Semi-amplitude (K2) (secondary) | 21.526±0.017 km/s |
| Details[2] | |
| γ CMi A | |
| Mass | 1.88 M☉ |
| Radius | 36.8±2.6 R☉ |
| Luminosity | 321±33 L☉ |
| Temperature | 4,036±100 K |
| Rotational velocity (v sin i) | 5±2 km/s |
| Age | 1.3 Gyr |
| γ CMi B | |
| Mass | 1.85 M☉ |
| Radius | 7.8±1.0 R☉ |
| Luminosity | 25.4±5.2 L☉ |
| Temperature | 4,658±200 K |
| Rotational velocity (v sin i) | 2.0±2.0 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Gamma Canis Minoris is a binary star system in the equatorial constellation Canis Minor. Its name is a Bayer designation that is Latinized from γ Canis Minoris, and abbreviated Gamma CMi or γ CMi. The orange colour is obvious when seen through binoculars.[7] The system is visible to the naked eye with a combined apparent visual magnitude of +4.33.[2] Based upon an annual parallax shift of 3.13 mas as seen from Earth,[1] this system is located at a distance of approximately 1,040 light-years (320 pc) from the Sun. It is drifting further away with a line of sight velocity of 47 km/s.[5]
This spectroscopic binary star system has an orbital period of 389.31 days, a semimajor axis of 1.48 AU, and an eccentricity of 0.2586.[2] Their variable radial velocity was discovered by H. M. Reese in 1902 at Lick Observatory.[8] Both components are evolved, K-type giant stars, most likely on their first ascent along the red giant branch. The primary, component A, has a stellar classification of K4 III while the secondary, component B, may be K1: III.[2]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
- ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 Fekel, F. C. et al. (March 2013), "The spectroscopic orbit of the K-giant binary γ Canis Minoris", Astronomische Nachrichten 334 (3): 223, doi:10.1002/asna.201211842, Bibcode: 2013AN....334..223F.
- ↑ Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series 71: 245, doi:10.1086/191373, Bibcode: 1989ApJS...71..245K.
- ↑ 4.0 4.1 Johnson, H. L. (1966), "UBVRIJKL Photometry of the Bright Stars", Communications of the Lunar and Planetary Laboratory 4: 99, Bibcode: 1966CoLPL...4...99J.
- ↑ 5.0 5.1 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics 546: 14, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ "gam CMi". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=gam+CMi.
- ↑ Kambič, Bojan (2009), Viewing the Constellations with Binoculars: 250+ Wonderful Sky Objects to See and Explore, Springer, p. 32, ISBN 978-0387853543, https://books.google.com/books?id=3vxLNPNHOcwC&pg=PA233.
- ↑ Campbell, W. W. (September 1902), "Six stars whose velocities in the line of sight are variable", Astrophysical Journal 16: 114–117, doi:10.1086/140954, Bibcode: 1902ApJ....16..114C.
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