Astronomy:35 Comae Berenices
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Coma Berenices |
| Right ascension | 12h 53m 17.74703s[1] |
| Declination | +21° 14′ 41.8092″[1] |
| Apparent magnitude (V) | 4.93[2] |
| Characteristics | |
| Spectral type | G5 III + F:[2] |
| U−B color index | 0.65[3] |
| B−V color index | 0.90[3] |
| Astrometry | |
| Radial velocity (Rv) | −6.091±0.075[4] km/s |
| Proper motion (μ) | RA: −37.66[1] mas/yr Dec.: −30.14[1] mas/yr |
| Parallax (π) | 11.52 ± 0.87[1] mas |
| Distance | 280 ± 20 ly (87 ± 7 pc) |
| Orbit[5] | |
| Period (P) | 539.4±95.4 yr |
| Semi-major axis (a) | 1.405±0.046″ |
| Eccentricity (e) | 0.208±0.100 |
| Inclination (i) | 28.4±13.4° |
| Longitude of the node (Ω) | 238.7±2.7° |
| Periastron epoch (T) | 1949.4±7.9 |
| Argument of periastron (ω) (secondary) | 251.6±7.3° |
| Other designations | |
| Database references | |
| SIMBAD | data |
35 Comae Berenices is a multiple star system in the northern constellation of Coma Berenices, located about 6° from the north galactic pole. It is faintly visible to the naked eye with an apparent visual magnitude of 4.93.[2] Based upon parallax measurements, it is located around 280 light years from the Sun.[1] The system is moving closer to the Earth with a heliocentric radial velocity of −6 km/s.[4]
This was found to be a wide binary by Struve in 1828,[3] but it has completed less than half an orbit since then and the orbital elements remain poorly constrained. It has an orbital period of 539±95 years and an eccentricity of 0.2±0.1.[5] The pair have been resolved into stellar classifications of an evolved G-type giant primary of class G5 III and an F-type secondary,[2] most likely main sequence with a class of F1 V.[3] The primary component is a spectroscopic binary[3] with a period of 7.9624 ± 0.0117 years and an eccentricity of 0.63.[4] A fourth component, 35 Com C, is located 29″ from the primary and may have a physical association.[3]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 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.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Griffin, R. F. et al. (March 1988), "The giant spectroscopic binary 35 Comae", Publications of the Astronomical Society of the Pacific 100: 358–361, doi:10.1086/132177, Bibcode: 1988PASP..100..358G.
- ↑ 4.0 4.1 4.2 Halbwachs, J.-L. et al. (May 2012), "Double stars with wide separations in the AGK3 - I. Components that are themselves spectroscopic binaries", Monthly Notices of the Royal Astronomical Society 422 (1): 14–24, doi:10.1111/j.1365-2966.2012.20308.x, Bibcode: 2012MNRAS.422...14H.
- ↑ 5.0 5.1 Drummond, Jack D. (March 2014), "Binary Stars Observed with Adaptive Optics at the Starfire Optical Range", The Astronomical Journal 147 (3): 10, doi:10.1088/0004-6256/147/3/65, 65, Bibcode: 2014AJ....147...65D.
- ↑ "35 Com". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=35+Com.
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