Astronomy:35 Cancri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[1] mas |
| 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
- ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 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, doi:10.1088/0004-6256/150/5/158, 158, Bibcode: 2015AJ....150..158Y
- ↑ 4.0 4.1 4.2 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, doi:10.1086/319956, Bibcode: 2001AJ....121.2148G.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 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, doi:10.1088/0004-637X/776/2/67, 67, Bibcode: 2013ApJ...776...67V.
- ↑ 6.0 6.1 Muñoz Bermejo, J. et al. (May 2013), "A PCA approach to stellar effective temperatures", Astronomy and Astrophysics 453: A95, doi:10.1051/0004-6361/201220961, Bibcode: 2013A&A...553A..95M.
- ↑ "35 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=35+Cnc.
- ↑ 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, doi:10.1088/0004-637X/784/1/57, 57, Bibcode: 2014ApJ...784...57W.
- ↑ van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review 20 (1): 51, doi:10.1007/s00159-012-0051-2, Bibcode: 2012A&ARv..20...51V.
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