HD 37756

Last updated
HD 37756
Orion constellation map.svg
Red circle.svg
Location of HD 37756 (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Orion
Right ascension 05h 40m 50.71498s [1]
Declination −01° 07′ 43.6366″ [1]
Apparent magnitude  (V)4.95 [2]
Characteristics
primary
Spectral type B2IV-V [3] or B3V [4]
U−B color index −0.83 [5]
B−V color index −0.21 [5]
secondary
Spectral type B1 [6]
Astrometry
Radial velocity (Rv)+26.10 [7]  km/s
Proper motion (μ)RA: −1.50 [1]   mas/yr
Dec.: −0.84 [1]   mas/yr
Parallax (π)3.63 ± 0.37  mas [1]
Distance approx. 900  ly
(approx. 280  pc)
Absolute magnitude  (MV)−2.74 [2]
Orbit [8]
Period (P)27.154925 d
Eccentricity (e)0.739±0.007
Periastron epoch (T)2447886.076±0.065  HJD
Argument of periastron (ω)
(secondary)		81.4±2.4°
Semi-amplitude (K1)
(primary)		84.7±1.1 km/s
Details
A
Mass 8.6±0.2 [9]   M☉
Radius 5.3 [10]   R☉
Luminosity 4,830 [11]   L☉
Surface gravity (log g)3.84 [10]   cgs
Temperature 21,150 [11]   K
Metallicity [Fe/H]+0.01 [12]   dex
Rotational velocity (v sin i)75 [13]  km/s
Age 18.0±3.2 [9]   Myr
B
Mass 8.3 [6]   M☉
Other designations
NSV  2556, BD−01°1004, GC  7091, HD  37756, HIP  26736, HR  1952, SAO  132445 [14]
Database references
SIMBAD data

HD 37756 is a binary star system in the equatorial constellation of Orion, positioned less than a degree to the north of the bright star Alnitak. [15] It has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.95. [2] The system is located at a distance of approximately 900  light years from the Sun based on parallax, [1] and is drifting further away with a radial velocity of +26 km/s. [7] It is a member of the OB1b subgroup of the Orion OB1 association. [16]

The binary nature of this system was identified by E. B. Frost in 1904. [17] It is a double-lined spectroscopic binary with an orbital period of 27.15 days and a high eccentricity of 0.74. [8] The spectrum matches a massive B-type main-sequence star with a stellar classification of B3V. [4] The secondary is luminous enough to interfere with measurements of the primary spectrum. [17] It is a suspected Cepheid variable with a period of 0.37968 days and an amplitude of 0.03 magnitude in the B band of the UBV photometric system. [18] The system is a candidate eclipsing binary with a minimum dip of 0.04 in visual magnitude during each orbit. [19]

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References

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  7. 1 2 Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institution for Science. Bibcode:1953GCRV..C......0W. LCCN   54001336.
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  11. 1 2 Hohle, M. M.; et al. (2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331 (4): 349. arXiv: 1003.2335 . Bibcode:2010AN....331..349H. doi:10.1002/asna.200911355. S2CID   111387483. Vizier catalog entry
  12. ↑ Gontcharov, G. A. (2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv: 1606.08814 . Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. S2CID   118345778. Vizier catalog entry
  13. ↑ Abt, Helmut A.; et al. (2002). "Rotational Velocities of B Stars". The Astrophysical Journal. 573 (1): 359–365. Bibcode:2002ApJ...573..359A. doi: 10.1086/340590 .
  14. ↑ "HD 37756". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-11-20.
  15. ↑ Sinnott, Roger W.; Perryman, Michael A. C. (1997). Millennium Star Atlas. Vol. 1. Sky Publishing Corporation and the European Space Agency. p. 253. ISBN   0-933346-84-0.
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  18. ↑ Hill, Graham (August 1967). "On Beta Cephei Stars: a Search for Beta Cephei Stars". Astrophysical Journal Supplement. 14: 263. Bibcode:1967ApJS...14..263H. doi: 10.1086/190156 .
  19. ↑ Hoffleit, Dorrit (1996). "A Catalogue of Correlations Between Eclipsing Binaries and Other Categories of Double Stars". The Journal of the American Association of Variable Star Observers. 24 (2): 105–116. Bibcode:1996JAVSO..24..105H.
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