Astronomy:15 Camelopardalis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[2] mas |
| 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
- ↑ 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. doi:10.1017/S1743921311026949. Bibcode: 2012IAUS..282...71B. https://www.researchgate.net/publication/232274903. Retrieved 9 November 2021.
- ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement 17: 371, doi:10.1086/190179, Bibcode: 1968ApJS...17..371L
- ↑ 5.0 5.1 5.2 5.3 5.4 Bakış, V. et al. (April 2012), "Northern Binaries in the Evrena Project", in Richards, M. T.; Hubeny, I., From Interacting Binaries to Exoplanets: Essential Modeling Tools, Proceedings of the International Astronomical Union, 282, pp. 71–72, doi:10.1017/S1743921311026949, Bibcode: 2012IAUS..282...71B.
- ↑ 6.0 6.1 6.2 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 64: pp. 397–398, doi:10.1051/eas/1364063.
- ↑ "15 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=15+Cam.
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