35 Cancri

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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]
Evolutionary stage subgiant[3]
Spectral type G0 III[4]
B−V color index +0.681±0.013[2]
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
Distance630 ± 7 ly
(193 ± 2 pc)
Absolute magnitude (MV)0.22[2]
Mass1.072[5] M
Radius0.981[5] R
Luminosity77.23[2] L
Temperature5,950[6] K
Rotation0.501 d[5]
Rotational velocity (v sin i)99.0[5] km/s
Other designations
35 Cnc, BD+20°2118, GC 11904, HD 72779, HIP 42133, HR 3387, SAO 97928[7]
Database references

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]


  1. ^ 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.
  2. ^ 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.
  3. ^ 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
  4. ^ 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.
  5. ^ 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.
  6. ^ 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.
  7. ^ "35 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-02-28.
  8. ^ 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.
  9. ^ 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.