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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
SIMBAD data

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 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. ^ a b c d e 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. ^ 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.
  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. ^ a b c d e f g h i 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.
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