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15 Camelopardalis

From Wikipedia, the free encyclopedia

15 Camelopardalis

A Hipparcos light curve for DV Camelopardalis, adapted from Bakiş et al. (2011)[1]
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]
Distance1,040 ± 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
Luminosity220.01[3] L☉
Other designations
15 Cam, DV Cam, BD+57°874, HD 34233, HIP 24836, HR 1719, SAO 25125[7]
Database references
SIMBADdata

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

  1. ^ 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.
  2. ^ 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.
  3. ^ 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.
  4. ^ 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
  5. ^ 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.
  6. ^ 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.
  7. ^ "15 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-16.
This page was last edited on 14 August 2023, at 21:25
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