35 Cancri
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cancer |
| Right ascension | 08h 35m 19.44616s[1] |
| Declination | +19° 35′ 24.2308″[1] |
| Apparent magnitude (V) | +6.55[2] |
| Characteristics | |
| Evolutionary stage | subgiant[3] |
| Spectral type | G0 III[4] |
| B−V color index | +0.681±0.013[2] |
| Astrometry | |
| Radial velocity (Rv) | +34.9±1.2[2] km/s |
| Proper motion (μ) | RA: −34.582[1] mas/yr Dec.: −12.417[1] mas/yr |
| Parallax (π) | 5.1788 ± 0.0588 mas[1] |
| Distance | 630 ± 7 ly (193 ± 2 pc) |
| Absolute magnitude (MV) | 0.22[2] |
| Details | |
| Mass | 1.072[5] M☉ |
| Radius | 0.981[5] R☉ |
| Luminosity | 77.23[2] L☉ |
| Temperature | 5,950[6] K |
| Rotation | 0.501 d[5] |
| Rotational velocity (v sin i) | 99.0[5] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
35 Cancri is a star in the zodiac constellation of Cancer, located 630 light years from the Sun. It is a challenge to view with the naked eye even under good seeing conditions, having an apparent visual magnitude of +6.55.[2] The star is moving further from the Earth with a heliocentric radial velocity of +35 km/s,[2] and is a member of the Beehive Cluster.[8]
This is a subgiant star[3] with a stellar classification of G0 III.[4] It is rotating at a relatively fast clip, giving it an oblate shape with an equatorial bulge that is 5% larger than the polar radius.[9] 35 Cancri has a projected rotational velocity of 99 km/s[5] and a rotation period of 0.5 days.[5] This rotation is expected to decrease significantly as the star expands into a giant.[4] It has nearly the same mass and size as the Sun,[5] but is radiating 77[2] times the Sun's luminosity from its photosphere at an effective temperature of 5,950 K.[6]
References
- ^ a b c d e 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 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.
- ^ a b Yang, X. L.; et al. (November 2015), "Chemical Abundances of Member Stars in the Open Cluster NGC 2632 (Praesepe)", The Astronomical Journal, 150 (5): 10, Bibcode:2015AJ....150..158Y, doi:10.1088/0004-6256/150/5/158, 158
- ^ a b c Gray, R. O.; et al. (2001), "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars", The Astronomical Journal, 121 (4): 2148, Bibcode:2001AJ....121.2148G, doi:10.1086/319956.
- ^ a b c d e f g van Saders, Jennifer L.; Pinsonneault, Marc H. (October 2013), "Fast Star, Slow Star; Old Star, Young Star: Subgiant Rotation as a Population and Stellar Physics Diagnostic", The Astrophysical Journal, 776 (2): 20, arXiv:1306.3701, Bibcode:2013ApJ...776...67V, doi:10.1088/0004-637X/776/2/67, 67.
- ^ a b Muñoz Bermejo, J.; et al. (May 2013), "A PCA approach to stellar effective temperatures", Astronomy and Astrophysics, 453: A95, arXiv:1303.7218, Bibcode:2013A&A...553A..95M, doi:10.1051/0004-6361/201220961.
- ^ "35 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-02-28.
- ^ Wang, P. F.; et al. (March 2014), "Characterization of the Praesepe Star Cluster by Photometry and Proper Motions with 2MASS, PPMXL, and Pan-STARRS", The Astrophysical Journal, 784 (1): 10, arXiv:1401.7424, Bibcode:2014ApJ...784...57W, doi:10.1088/0004-637X/784/1/57, 57.
- ^ van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2.
