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Beta Camelopardalis, Latinised 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 −1.90 km/s[4] and is most likely a single[10] star.

β Camelopardalis
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]
Characteristics
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]
Astrometry
Radial velocity (Rv)−1.90[4] km/s
Proper motion (μ) RA: −6.50[1] mas/yr
Dec.: −14.15[1] mas/yr
Parallax (π)3.74 ± 0.21 mas[1]
Distance870 ± 50 ly
(270 ± 20 pc)
Absolute magnitude (MV)−3.1[5]
Details
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
Age53[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
SIMBADdata
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

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 arcseconds; and a 12th-magnitude star at 15 arcseconds.[13]


References


  1. Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. 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. 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. Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
  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. 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. S2CID 118372600.
  7. 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: 343–357. arXiv:1208.2037. Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x. S2CID 118665352.
  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. S2CID 118683158.
  9. 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. S2CID 119271718.
  10. 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.
  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. S2CID 119271718. 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, S2CID 119267456
  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.



На других языках

[de] Beta Camelopardalis

β Camelopardalis (Beta Camelopardalis, kurz β Cam) ist mit einer scheinbaren Helligkeit von 4,03m der hellste Stern des Sternbildes Giraffe (lateinisch Camelopardalis). Dennoch erscheint er dem bloßen Auge nur als lichtschwaches Objekt. Seine Entfernung zur Erde beträgt nach neuen, im Dezember 2020 veröffentlichten Auswertungen der Messergebnisse der Raumsonde Gaia etwa 840 Lichtjahre.[1] Zu einem relativ ähnlichen Resultat, nämlich einer Entfernung von circa 870 Lichtjahren, führte bereits eine 2007 vorgestellte Validierung der Messwerte der Vorgängermission Hipparcos.[8] β Camelopardalis ist weit genug entfernt und nahe genug der Milchstraße, als dass seine scheinbare Helligkeit aufgrund von zwischen der Erde und dem Stern liegenden, seine Strahlung teilweise absorbierenden interstellaren Staub um 15 Prozent geschwächt erscheint.[2]
- [en] Beta Camelopardalis

[es] Beta Camelopardalis

Beta Camelopardalis (β Cam / 10 Camelopardalis / HD 31910) es la estrella más brillante de la constelación de Camelopardalis —la jirafa— con magnitud aparente +4,03.[1] De acuerdo a su paralaje (3,74 milisegundos de arco),[1] se encuentra a 870 años luz de distancia del Sistema Solar.

[ru] Бета Жирафа

Бета Жирафа (β Cam / β Camelopardalis) — ярчайшая звезда в созвездии Жирафа.


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