HD 37017

HD 37017

A light curve for V1046 Orionis, plotted from TESS data
Observation data
Epoch J2000      Equinox ICRS
Constellation Orion
Right ascension 05h 35m 21.86770s
Declination −04° 29′ 39.0409″
Apparent magnitude (V) 6.555 – 6.571
Characteristics
Evolutionary stage B2/3V (B1.5 Vp He strong)
U−B color index −0.79
B−V color index −0.14
Variable type SX Ari
Astrometry
Radial velocity (Rv)+32±2 km/s
Proper motion (μ) RA: 1.88±0.09 mas/yr
Dec.: 1.20±0.14 mas/yr
Parallax (π)2.643±0.075 mas
Distance1,230 ± 40 ly
(380 ± 10 pc)
Absolute magnitude (MV)−1.2
Orbit
Period (P)18.6556±0.0017 d
Semi-major axis (a)≥12.61±1.09 R☉
Eccentricity (e)0.31±0.05
Periastron epoch (T)2,435,461.602±0.168 JD
Argument of periastron (ω)
(secondary)		133±5°
Semi-amplitude (K1)
(primary)		36.0±2.5 km/s
Details
A
Mass8.50±0.53 M☉
Luminosity3,754 L☉
Temperature23,700 K
Rotation0.901 d
Rotational velocity (v sin i)165 km/s
B
Mass4.5 M☉
Other designations
V1046 Orionis, BD−04°1183, HD 37017, HIP 26233, HR 1890, SAO 132317
Database references
SIMBADdata

HD 37017 is a binary star system in the equatorial constellation of Orion. It has the variable star designation V1046 Orionis; HD 37017 is the identifier from the Henry Draper Catalogue. The system is a challenge to view with the naked eye, being close to the lower limit of visibility with a combined apparent visual magnitude of 6.6. It is located at a distance of approximately 1,230 light years based on parallax, and is drifting further away with a radial velocity of +32 km/s. The system is part of star cluster NGC 1981.

The binary nature of this system was suggested by A. Blaauw and T. S. van Albada in 1963. It is a double-lined spectroscopic binary with an orbital period of 18.6556 days and an eccentricity of 0.31. The eccentricity is considered unusually large for such a close system. It has been suspected of being an eclipsing binary or rotating ellipsoidal variable, and the primary is also am SX Arietis variable.

The primary is a helium-strong, magnetic chemically peculiar star with a stellar classification of B1.5 Vp. It has a magnetic field strength of 7,700 G, and the helium concentrations are located at the magnetic poles. V1046 Orionis was found to be a variable star by L. A. Balona in 1997, and is now classified as an SX Arietis variable. The star undergoes periodic changes in visual brightness, magnetic field strength, and spectral characteristics with a cycle time of 0.901175 days – the star's presumed rotation period. Radio emission has been detected that varies with the rotation period.

The secondary component has an estimated 4.5 times the mass of the Sun. The class has been estimated as type B6III-IV.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 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. XHIP record for this object at VizieR.
  3. 1 2 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.
  4. ↑ "V1046 Ori". International Variable Star Index. AAVSO. Retrieved 2025-11-04.
  5. ↑ Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
  6. 1 2 3 Abt, Helmut A.; et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590.
  7. 1 2 Walker, M. F. (February 1969), "Studies of extremely young clusters. V. Stars in the vicinity of the Orion nebula", Astrophysical Journal, 155: 447, Bibcode:1969ApJ...155..447W, doi:10.1086/149881.
  8. 1 2 3 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  9. 1 2 Blaauw, A.; et al. (April 1963), "Radial Velocities of B-Type Stars in the Nearest Associations.", Astrophysical Journal, 137: 791, Bibcode:1963ApJ...137..791B, doi:10.1086/147556.
  10. 1 2 3 4 Kounkel, Marina; et al. (2017), "The Gould's Belt Distances Survey (GOBELINS) II. Distances and Structure toward the Orion Molecular Clouds", The Astrophysical Journal, 834 (2), 142, arXiv:1609.04041, Bibcode:2017ApJ...834..142K, doi:10.3847/1538-4357/834/2/142, hdl:1887/59417, S2CID 26439367.
  11. 1 2 3 Leone, F.; Catanzaro, G. (March 1999), "Orbital elements of binary systems with a chemically peculiar star", Astronomy and Astrophysics, 343: 273–280, Bibcode:1999A&A...343..273L.
  12. 1 2 3 Hohle, M. M.; et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349–360, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
  13. 1 2 3 4 5 6 Bolton, C. T.; et al. (September 1998), "HD 37017 = V 1046 ORI A double-lined spectroscopic binary with a B2e He-strong magnetic primary", Astronomy and Astrophysics, 337: 183–197, Bibcode:1998A&A...337..183B.
  14. ↑ "V1046 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-31.
  15. ↑ Maia, F. F. S.; et al. (September 2010), "Characterization and photometric membership of the open cluster NGC1981", Monthly Notices of the Royal Astronomical Society, 407 (3): 1875–1886, arXiv:1005.3047, Bibcode:2010MNRAS.407.1875M, doi:10.1111/j.1365-2966.2010.17034.x, S2CID 119206669.
  16. ↑ Ducati, J. R.; et al. (January 2011), "The mass ratio and initial mass functions in spectroscopic binaries" (PDF), Astronomy and Astrophysics, 525: 9, Bibcode:2011A&A...525A..26D, doi:10.1051/0004-6361/200913895, hdl:10183/99264, A26.
  17. ↑ Ghazaryan, S.; et al. (August 2019), "Statistical analysis of roAp, He-weak, and He-rich stars", Monthly Notices of the Royal Astronomical Society, 487 (4): 5922–5931, arXiv:1906.06984, Bibcode:2019MNRAS.487.5922G, doi:10.1093/mnras/stz1678, S2CID 189928323.
  18. ↑ Trigilio, C.; et al. (May 2004), "A three-dimensional model for the radio emission of magnetic chemically peculiar stars", Astronomy and Astrophysics, 418 (2): 593–605, arXiv:astro-ph/0402432, Bibcode:2004A&A...418..593T, doi:10.1051/0004-6361:20040060, S2CID 15884571.
  19. 1 2 Leone, F.; Umana, G. (January 1993), Dworetsky, M. M.; Castelli, F.; Faraggiana, R. (eds.), "Periodic Radio Emission from the Helium Rich Stars HD 37017 and σ Ori E", Peculiar versus Normal Phenomena in A-type and Related Stars. International Astronomical Union, Colloquium No. 138, held in Trieste, Italy, July 1992, vol. 44, no. 138, San Francisco: Astronomical Society of the Pacific, p. 541, Bibcode:1993ASPC...44..541L.