HD 90264

HD 90264 is a binary star[4] system in the southern constellation of Carina. It has the Bayer designation of L Carinae, while HD 90264 is the star's identifier in the Henry Draper catalogue. This system has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.97.[2] It is located at a distance of approximately 402 light years from the Sun based on parallax, and is drifting further away with a radial velocity of around +12 km/s.[2] The system is a member of the Lower Centaurus Crux association of the Sco-Cen Complex.[4]

This article is about L Carinae. For l Carinae, see HD 84810.
HD 90264
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Carina
Right ascension 10h 22m 58.14606s[1]
Declination −66° 54′ 05.3903″[1]
Apparent magnitude (V) 4.97[2]
Characteristics
Spectral type B8V[3]
B−V color index −0.128±0.003[2]
Astrometry
Radial velocity (Rv)+12.0±4.2[2] km/s
Proper motion (μ) RA: −22.39[1] mas/yr
Dec.: +11.48[1] mas/yr
Parallax (π)8.12 ± 0.18 mas[1]
Distance402 ± 9 ly
(123 ± 3 pc)
Absolute magnitude (MV)−0.403[4]
Orbit[4]
Period (P)15.727±0.001 d
Semi-major axis (a)52.66 R☉
Eccentricity (e)0.044±0.014
Inclination (i)54°
Periastron epoch (T)2,452,814.78±1.05 JD
Argument of periastron (ω)
(secondary)		138±25°
Semi-amplitude (K1)
(primary)		62.2±1.9 km/s
Semi-amplitude (K2)
(secondary)		76.0±1.5 km/s
Details
A
Mass4.3[4] M☉
Luminosity288.39[2] L☉
Rotational velocity (v sin i)7[4] km/s
Age18[4] Myr
B
Mass3.5[4] M☉
Other designations
L Car, CPD−66°1243, FK5 2834, GC 14283, HD 90264, HIP 50847, HR 4089, SAO 250940[5]
Database references
SIMBADdata

This system was found to be a close double-lined spectroscopic binary in 1977, consisting of two B-type main-sequence stars. It has a near circular orbit with a period of 15.727 days and a semimajor axis of 0.2449 AU. They appear to be spin-orbit synchronized. Both stars appear to be deficient in helium. The primary is a helium variable star while the companion is a mercury-manganese star. The variability of both stars aligns favorably with the orbital period.[4]

References
  1. van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  2. 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.
  3. Houk, Nancy; Cowley, A. P. (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
  4. Quiroga, C.; et al. (October 2010), "The chemically peculiar double-lined spectroscopic binary HD 90264", Astronomy and Astrophysics, 521: 7, Bibcode:2010A&A...521A..75Q, doi:10.1051/0004-6361/201014521, A75.
  5. "HD 90264". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-01-26.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.