15 Camelopardalis
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 05h 19m 27.85996s[2] |
| Declination | +58° 07′ 02.5203″[2] |
| Apparent magnitude (V) | 6.13[3] |
| Characteristics | |
| Spectral type | B5 V[4] |
| B−V color index | −0.031±0.005[3] |
| Variable type | Algol,[5] SPB[6] |
| Astrometry | |
| Radial velocity (Rv) | 6.7±3.7[3] km/s |
| Proper motion (μ) | RA: +5.558[2] mas/yr Dec.: −18.832[2] mas/yr |
| Parallax (π) | 3.1406 ± 0.0571 mas[2] |
| Distance | 1,040 ± 20 ly (318 ± 6 pc) |
| Absolute magnitude (MV) | −0.74[3] |
| Orbit[5] | |
| Period (P) | 6.6784±0.0010 d |
| Eccentricity (e) | ~0.48 |
| Details | |
| Luminosity | 220.01[3] L☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
15 Camelopardalis is a triple star[5] system in the northern circumpolar constellation of Camelopardalis. It has the variable star designation DV Camelopardalis; 15 Camelopardalis is the Flamsteed designation. This is just visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of 6.13.[3] It is a probable (99%) member of the Cas-Tau OB association.[5]
This system includes a double-lined spectroscopic binary with an orbital period of 6.7 days and a large eccentricity of around 0.48, plus a third component in a wider orbit. The close pair consist of a very slowly rotating helium-weak star plus an ordinary mid-B-type star with a more rapid rotation rate.[6] Together they form an Algol-type eclipsing binary with a depth of about 0.2 magnitude.[5] The third component is a slowly pulsating B-type star.[6]
References
[edit]- ^ Bakiş, V.; Hensberge, H.; Zejda, M.; de Cat, P.; Yılmaz, F.; Bloemen, S.; Svoboda, P.; Demircan, O. (April 2012). "Northern Binaries in the Evrena Project". From Interacting Binaries to Exoplanets: Essential Modeling Tools Proceedings IAU Symposium No. 282. 282: 71–72. Bibcode:2012IAUS..282...71B. doi:10.1017/S1743921311026949. Retrieved 9 November 2021.
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d e f 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, S2CID 119257644.
- ^ Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement, 17: 371, Bibcode:1968ApJS...17..371L, doi:10.1086/190179
- ^ a b c d e Bakış, V.; et al. (April 2012), "Northern Binaries in the Evrena Project", in Richards, M. T.; Hubeny, I. (eds.), From Interacting Binaries to Exoplanets: Essential Modeling Tools, Proceedings of the International Astronomical Union, vol. 282, pp. 71–72, Bibcode:2012IAUS..282...71B, doi:10.1017/S1743921311026949.
- ^ a b c Hensberge, H.; et al. (February 25, 2014), Pavlovski, K.; Tkachenko, A.; Torres, G. (eds.), "The triple B–star system DV Cam", Setting a New Standard in the Analysis of Binary Stars, EAS Publications Series, vol. 64, pp. 397–398, doi:10.1051/eas/1364063.
- ^ "15 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-16.
