HD 37756

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HD 37756
Orion constellation map.svg
Red circle.svg
Location of HD 37756 (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Orion [1]
Right ascension 05h 40m 50.71498s [2]
Declination −01° 07′ 43.6366″ [2]
Apparent magnitude  (V)4.95 [1]
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 [2] mas/yr
Dec.: −0.84 [2] mas/yr
Parallax (π)3.63±0.37  mas [2]
Distance approx. 900  ly
(approx. 280  pc)
Absolute magnitude  (MV)−2.74 [1]
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 13.0 [6]   M☉
B
Mass 8.3 [6]   M☉
Other designations
NSV 2556, BD−01°1004, GC 7091, HD 37756, HIP 26736, HR 1952, SAO 132445 [9]
Database references
SIMBAD data
HD 37756, due north of Alnitak, the bright star at the centre of the frame, and due east (left) of Alnilam, the bright star on the right Spectacular visible light wide-field view of region of Orion's Belt and the Flame Nebula.jpg
HD 37756, due north of Alnitak, the bright star at the centre of the frame, and due east (left) of Alnilam, the bright star on the right

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. [10] It has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.95. [1] The system is located at a distance of approximately 900  light years from the Sun based on parallax, [2] 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. [11]

The binary nature of this system was identified by E. B. Frost in 1906. [12] 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. [12] It is a suspected Beta Cephei variable with a period of 0.37968 days and an amplitude of 0.03 magnitude in the B band of the UBV photometric system. [13] The system is a candidate eclipsing binary with a minimum dip of 0.04 in visual magnitude during each orbit. [14]

References

  1. 1 2 3 4 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. XHIP record for this object at VizieR.
  2. 1 2 3 4 5 6 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. S2CID   18759600. Vizier catalog entry
  3. ↑ Hoffleit, D.; Warren, W. H. (1995). "Bright Star Catalogue". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050 (5th Revised ed.). Bibcode:1995yCat.5050....0H.
  4. 1 2 Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
  5. 1 2 Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers. 42 (2): 443. Bibcode:2014JAVSO..42..443M. Vizier catalog entry
  6. 1 2 3 Kraicheva, Z.; Popova, E.; Tutukov, A.; Yungelson, L. (July 1980). "Catalogue of physical parameters of spectroscopic binary stars". Bulletin d'Information du Centre de Donnees Stellaires. 19: 71. Bibcode:1980BICDS..19...71K. ISSN   1169-8837.
  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.
  8. 1 2 Hilditch, R. W.; et al. (February 1991). "The eccentric-orbit binaries Iota Orionis and HR 1952: a cautionary tale". The Observatory. 111: 14–20. Bibcode:1991Obs...111...14H.
  9. ↑ "HD 37756". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-11-20.
  10. ↑ 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.
  11. ↑ Voss, R.; et al. (September 2010). "Probing the evolving massive star population in Orion with kinematic and radioactive tracers". Astronomy and Astrophysics. 520: 10. arXiv: 1005.3827 . Bibcode:2010A&A...520A..51V. doi:10.1051/0004-6361/201014408. S2CID   38599952. A51.
  12. 1 2 Rao, N. Kameswara; et al. (1990). "The eccentric double-lined binary BD — 1° 1004". Journal of Astrophysics and Astronomy. 11 (4): 445. Bibcode:1990JApA...11..445K. doi:10.1007/BF02709760. S2CID   73616576.
  13. ↑ 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 .
  14. ↑ 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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