Gamma Camelopardalis
  | |
| 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 | |
| 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 is a suspected wide binary star[10] 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]
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.
- ^ 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.
