83 Cancri is an astrometric binary[6][7] star system in the northern constellation of Cancer, positioned near the constellation border with Leo. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.61.[2] Despite having a Flamsteed designation, the system was too faint to be included in the Bright Star Catalogue.[8] It is located at a distance of 133 light years from the Sun, based on parallax,[1] but is drifting closer with a radial velocity of −15 km/s.[2] 83 Cancri has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.185″ per annum.[9]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cancer |
| Right ascension | 09h 18m 58.82772s[1] |
| Declination | +17° 42′ 19.2744″[1] |
| Apparent magnitude (V) | 6.61[2] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | F4V[2] + WD[3] |
| B−V color index | 0.487±0.030[2] |
| Variable type | constant[2] |
| Astrometry | |
| Radial velocity (Rv) | −14.8±0.4[2] km/s |
| Proper motion (μ) | RA: −135.130[1] mas/yr Dec.: −105.267[1] mas/yr |
| Parallax (π) | 24.5641 ± 0.0966 mas[1] |
| Distance | 132.8 ± 0.5 ly (40.7 ± 0.2 pc) |
| Absolute magnitude (MV) | 3.57[2] |
| Orbit[3] | |
| Period (P) | 32±2.5 d |
| Eccentricity (e) | 0.6±0.2 |
| Inclination (i) | 94±6° |
| Longitude of the node (Ω) | 148±5° |
| Periastron epoch (T) | 1976.0±3.5 |
| Argument of periastron (ω) (secondary) | 351±42° |
| Details | |
| 83 Cnc A | |
| Mass | 1.13[4] M☉ |
| Radius | 1.53+0.02 −0.05[1] R☉ |
| Luminosity | 3.135±0.015[1] L☉ |
| Surface gravity (log g) | 3.99[4] cgs |
| Temperature | 6,218+96 −53[1] K |
| Metallicity [Fe/H] | −0.26±0.02[2] dex |
| Age | 3.1[4] Gyr |
| 83 Cnc B | |
| Mass | 1.3[3] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
The pair have an orbital period of around 32 days and an eccentricity of about 0.6.[3] The visible member of this system, designated component A, is an F-type main-sequence star with a stellar classification of F4V.[2] Its atmosphere is enhanced with s-process elements, particularly strontium and yttrium, which is attributed to mass transfer from the companion while the latter was on the asymptotic giant branch.[10] The primary is 3.1[4] billion years old with 1.1[4] times the mass of the Sun and 1.5[1] times the Sun's radius. It is radiating 3.1[1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,218 K.[1] The unseen secondary companion is most likely a high mass white dwarf, having around 1.3 times the Sun's mass.[3]
References edit
- ^ a b c d e f g h i j k l 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 e f g h i j 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.
- ^ a b c d e Goncharov, G. A.; Kiyaeva, O. V. (April 2002), "Astrometric Orbits from a Direct Combination of Ground-Based Catalogs with the Hipparcos Catalog", Astronomy Letters, 28 (4): 261–271, Bibcode:2002AstL...28..261G, doi:10.1134/1.1467262, S2CID 121692881.
- ^ a b c d e David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
- ^ "83 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 19 August 2017.
- ^ Tokovinin, Andrei (April 2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 14, arXiv:1401.6827, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, S2CID 56066740, 87.
- ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ Bidelman, W. P. (December 1990), "Flamsteed stars not contained in the Yale "Catalogue of Bright Stars"", Bulletin d'Information du Centre de Données Stellaires, 38: 13, Bibcode:1990BICDS..38...13B.
- ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv:astro-ph/0412070, Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID 2603568.
- ^ Reddy, Bacham E.; et al. (March 2003), "The chemical compositions of Galactic disc F and G dwarfs", Monthly Notices of the Royal Astronomical Society, 340 (1): 304–340, arXiv:astro-ph/0211551, Bibcode:2003MNRAS.340..304R, doi:10.1046/j.1365-8711.2003.06305.x, S2CID 14388692.