Astronomy:Beta Camelopardalis
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 05h 03m 25.091s[1] |
| Declination | +60° 26′ 32.08″[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: −5.561[1] mas/yr Dec.: −14.400[1] mas/yr |
| Parallax (π) | 3.8800 ± 0.1635[1] mas |
| Distance | 840 ± 40 ly (260 ± 10 pc) |
| Absolute magnitude (MV) | −3.1[5] |
| Details | |
| Mass | 6.5[3] M☉ |
| Radius | 58±13[6] R☉ |
| Luminosity | 1,592[7] L☉ |
| Surface gravity (log g) | 1.79[3] cgs |
| Temperature | 5,300[3] K |
| Metallicity [Fe/H] | −0.06[8] dex |
| Rotational velocity (v sin i) | 11.7[9] km/s |
| Age | 53[3] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Data sources: | |
| Hipparcos Catalogue, CCDM (2002), Bright Star Catalogue (5th rev. ed.) | |
Beta Camelopardalis is the brightest star in the northern constellation of Camelopardalis. Its name is a Bayer designation that is Latinised from β Camelopardalis, and abbreviated Beta Cam or β Cam. This star 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 at a distance of approximately 840 light-years (260 pc) 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.
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 times the mass of the Sun[3] and has expanded to around 58 the Sun's radius.[6] The star is radiating 1,592 times the Sun's luminosity from its enlarged photosphere[7] 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
- ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 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.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 Lyubimkov, Leonid S. et al. (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. doi:10.1093/mnras/stu2299. Bibcode: 2015MNRAS.446.3447L.
- ↑ 4.0 4.1 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G.
- ↑ Gray, David F.; Pugh, Teznie (2012). "The Third Signature of Granulation in Bright-giant and Supergiant Stars". The Astronomical Journal 143 (4): 92. doi:10.1088/0004-6256/143/4/92. Bibcode: 2012AJ....143...92G.
- ↑ 6.0 6.1 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. doi:10.1111/j.1365-2966.2008.14146.x. Bibcode: 2009MNRAS.394.1925V.
- ↑ 7.0 7.1 McDonald, I. et al. (2012). "Fundamental parameters and infrared excesses of Hipparcos stars". Monthly Notices of the Royal Astronomical Society 427 (1): 343–357. doi:10.1111/j.1365-2966.2012.21873.x. Bibcode: 2012MNRAS.427..343M.
- ↑ Kovtyukh, V. V. et al. (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. doi:10.1111/j.1365-2966.2012.21117.x. Bibcode: 2012MNRAS.423.3268K.
- ↑ 9.0 9.1 Rodrigues Da Silva, R. et al. (2015). "On the Nature of Rapidly Rotating Single Evolved Stars". The Astrophysical Journal 801 (1): 54. doi:10.1088/0004-637X/801/1/54. Bibcode: 2015ApJ...801...54R.
- ↑ 10.0 10.1 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. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E.
- ↑ Rodrigues da Silva, R. et al. (March 2015). "On the Nature of Rapidly Rotating Single Evolved Stars". The Astrophysical Journal 801 (1): 6. doi:10.1088/0004-637X/801/1/54. 54. Bibcode: 2015ApJ...801...54R.
- ↑ 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. doi:10.1088/0067-0049/184/1/138. Bibcode: 2009ApJS..184..138H.
- ↑ Mason, Brian D. et al. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode: 2001AJ....122.3466M.
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