Beta Camelopardalis

β Camelopardalis
Camelopardalis constellation map.svg
Red circle.svg
Location of β Cam (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Camelopardalis
Right ascension  05h 03m 25.08963s[1]
Declination +60° 26′ 32.0895″[1]
Apparent magnitude (V) 4.02[2]
Spectral type G1Ib–IIa[3]
U−B color index +0.62[2]
B−V color index +0.93[2]
R−I color index +0.49[2]
Radial velocity (Rv)−190[4] km/s
Proper motion (μ) RA: −6.50[1] mas/yr
Dec.: −14.15[1] mas/yr
Parallax (π)3.74 ± 0.21[1] mas
Distance870 ± 50 ly
(270 ± 20 pc)
Absolute magnitude (MV)−3.1[5]
Mass6.5[3] M
Radius58±13[6] R
Luminosity1,592[7] L
Surface gravity (log g)1.79[3] cgs
Temperature5,300[3] K
Metallicity [Fe/H]−0.06[8] dex
Rotational velocity (v sin i)11.7[9] km/s
Age63[3] Myr
Other designations
β Cam, 10 Camelopardalis, BD+60° 856, FK5 182, HD 31910, HIP 23522, HR 1603, SAO 13351, ADS 3615 A, WDS J05034+6027
Database references
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

Beta Camelopardalis, Latinized from β Camelopardalis, is the brightest star in the northern constellation of Camelopardalis. It is bright enough to be faintly visible to the naked eye, having an apparent visual magnitude of 4.02.[2] Based upon an annual parallax shift of 3.74 mas as seen from Earth, it is located roughly 870 light years from the Sun. It is moving closer with a radial velocity of −190 km/s[4] and is most likely a single[10] star.

This is a yellow-hued G-type supergiant/bright giant with a stellar classification of G1 Ib–IIa.[3] It is an estimated 60 million years old and is spinning with a projected rotational velocity of 11.7 km/s.[9] This is an unusually high rate of rotation for an evolved star of this type. One possible explanation is that it may have engulfed a nearby giant planet, such as a hot Jupiter.[11]

Beta Camelopardalis has 6.5[3] times the mass of the Sun and has expanded to around 58[6] the Sun's radius. The star is radiating 1,592[7] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,300 K.[3] It is a source of X-ray emission.[12]

β Cam has two visual[10] companions: a 7th magnitude A5-class star at an angular separation of 84 arc seconds; and a 12th magnitude star at 15 arc seconds.[13]


  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. ^ a b c d e Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. ^ a b c d e f g h Lyubimkov, Leonid S.; Lambert, David L.; Korotin, Sergey A.; Rachkovskaya, Tamara M.; Poklad, Dmitry B. (2015). "Carbon abundance and the N/C ratio in atmospheres of A-, F- and G-type supergiants and bright giants". Monthly Notices of the Royal Astronomical Society. 446 (4): 3447. arXiv:1411.2722. Bibcode:2015MNRAS.446.3447L. doi:10.1093/mnras/stu2299.
  4. ^ a b Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065.
  5. ^ Gray, David F.; Pugh, Teznie (2012). "The Third Signature of Granulation in Bright-giant and Supergiant Stars". The Astronomical Journal. 143 (4): 92. Bibcode:2012AJ....143...92G. doi:10.1088/0004-6256/143/4/92.
  6. ^ a b Van Belle, G. T.; et al. (2009). "Supergiant temperatures and linear radii from near-infrared interferometry". Monthly Notices of the Royal Astronomical Society. 394 (4): 1925. arXiv:0811.4239. Bibcode:2009MNRAS.394.1925V. doi:10.1111/j.1365-2966.2008.14146.x.
  7. ^ a b McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012). "Fundamental parameters and infrared excesses of Hipparcos stars". Monthly Notices of the Royal Astronomical Society. 427: 343. arXiv:1208.2037. Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x.
  8. ^ Kovtyukh, V. V.; Gorlova, N. I.; Belik, S. I. (2012). "Accurate luminosities from the oxygen λ7771-4 Å triplet and the fundamental parameters of F-G supergiants". Monthly Notices of the Royal Astronomical Society. 423 (4): 3268. arXiv:1204.4115. Bibcode:2012MNRAS.423.3268K. doi:10.1111/j.1365-2966.2012.21117.x.
  9. ^ a b Rodrigues Da Silva, R.; Canto Martins, B. L.; De Medeiros, J. R. (2015). "On the Nature of Rapidly Rotating Single Evolved Stars". The Astrophysical Journal. 801: 54. arXiv:1503.03447. Bibcode:2015ApJ...801...54R. doi:10.1088/0004-637X/801/1/54.
  10. ^ a b 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.
  11. ^ Rodrigues da Silva, R.; Canto Martins, B. L.; De Medeiros, J. R. (March 2015). "On the Nature of Rapidly Rotating Single Evolved Stars". The Astrophysical Journal. 801 (1): 6. arXiv:1503.03447. Bibcode:2015ApJ...801...54R. doi:10.1088/0004-637X/801/1/54. 54.
  12. ^ Haakonsen, Christian Bernt; Rutledge, Robert E. (September 2009), "XID II: Statistical Cross-Association of ROSAT Bright Source Catalog X-ray Sources with 2MASS Point Source Catalog Near-Infrared Sources", The Astrophysical Journal Supplement, 184 (1): 138–151, arXiv:0910.3229, Bibcode:2009ApJS..184..138H, doi:10.1088/0067-0049/184/1/138
  13. ^ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.

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