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Gamma Camelopardalis
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| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Camelopardalis[1] |
| Right ascension | 03h 50m 21.509s[2] |
| Declination | +71° 19′ 56.16″[2] |
| Apparent magnitude (V) | 4.66[3] + 9.07[4] |
| Characteristics | |
| Spectral type | A2 IVn[5] |
| U−B color index | +0.07[3] |
| B−V color index | +0.03[3] |
| Astrometry | |
| Radial velocity (Rv) | −2.84±0.28[2] km/s |
| Proper motion (μ) | RA: +18.435 mas/yr[2] Dec.: −41.956 mas/yr[2] |
| Parallax (π) | 8.4446±0.0826 mas[2] |
| Distance | 386 ± 4 ly (118 ± 1 pc) |
| Absolute magnitude (MV) | −0.62[1] |
| Details | |
| γ Cam A | |
| Mass | 3.40±0.17[6] M☉ |
| Radius | 5.55±0.28[6] R☉ |
| Luminosity | 185[7] L☉ |
| Surface gravity (log g) | 3.70±0.01[2] cgs |
| Temperature | 8,892[7] K |
| Rotational velocity (v sin i) | 205[8] km/s |
| Other designations | |
| Shaowei, γ Cam, BD+70°259, FK5 138, GC 4557, HD 23401, HIP 17959, HR 1148, SAO 5006, CCDM 03504+7120, WDS J03504+7120A[9] | |
| Database references | |
| SIMBAD | data |
Gamma Camelopardalis, also named Shaowei,[10] is a suspected wide binary star[11] system in the northern circumpolar constellation of Camelopardalis. Its name is a Bayer designation that is Latinized from γ Camelopardalis, and abbreviated Gamma Cam or γ Cam. With a visual magnitude of 4.66,[3] it is faintly visible to the naked eye. Based upon an annual parallax shift of 9.09 mas as seen from Earth,[2] this system is located about 386 light-years (118 pc) from the Sun. It is drifting closer with a line of sight velocity of −2.8 km/s.[2]
The brighter primary, designated component A, is a white-hued A-type subgiant star with a stellar classification of A2 IVn.[5] It is spinning rapidly with a projected rotational velocity of 205 km/s. This is giving the star an oblate shape with an equatorial bulge that is 17% larger than the polar radius.[8] It has about 3.4 times the mass of the Sun and 5.6 times the Sun's radius.[6] The star is radiating 185[7] times the Sun's luminosity from its photosphere at an effective temperature of 8,892 K.[7]
The magnitude 9.07 secondary, BD+70 260, designated component C, lies at an angular separation of 106.00 arc seconds along a position angle of 85°, as of 2011. Component B is a magnitude 12.40 visual companion at a separation of 56.30 arc seconds along position angle 247°.[4]
In Chinese astronomy, the sixth star in the right wall of the Purple Forbidden Enclosure is named Shào Wèi (The Second Imperial Guard, 少衛). While its identification varies across historical sources, it is consistently in Camelopardalis; it was identified as γ Camelopardalis in the Yuan dynasty, but as α Camelopardalis in more recent sources.[12] The IAU Working Group on Star Names approved the name Shaowei for γ Camelopardalis A on 25 December 2025, and it is now so entered in the IAU Catalog of Star Names.[10]
References
[edit]- ^ a b 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. XHIP record for this object at VizieR.
- ^ a b c d e f g h Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
- ^ a b Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
- ^ a b Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
- ^ a b c Kervella, Pierre; et al. (2019), "Stellar and substellar companions of nearby stars from Gaia DR2: Binarity from proper motion anomaly", Astronomy & Astrophysics, 623: A72, arXiv:1811.08902, Bibcode:2019A&A...623A..72K, doi:10.1051/0004-6361/201834371, ISSN 0004-6361.
- ^ a b c d Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
- ^ a b 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, S2CID 119273474.
- ^ "gam Cam", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-09-08.
- ^ a b "IAU Catalog of Star Names". Retrieved 28 December 2025.
- ^ 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.
- ^ "Shaowei (少衛)". All Skies Encyclopaedia. IAU Working Group on Star Names. Retrieved 28 December 2025.
