HD 37017

Last updated
HD 37017
V1046OriLightCurve.png
A light curve for V1046 Orionis, plotted from TESS data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Orion [2]
Right ascension 05h 35m 21.86770s [3]
Declination −04° 29′ 39.0409″ [3]
Apparent magnitude  (V)6.555 –6.571 [4]
Characteristics
Evolutionary stage B2/3V [5] (B1.5 Vp He strong [6] )
U−B color index −0.79 [7]
B−V color index −0.14 [7]
Variable type SX Ari [8]
Astrometry
Radial velocity (Rv)+32±2 [9] km/s
Proper motion (μ)RA: 1.88±0.09 [10] mas/yr
Dec.: 1.20±0.14 [10] mas/yr
Parallax (π)2.643±0.075  mas [10]
Distance 1,230 ± 40  ly
(380 ± 10  pc)
Absolute magnitude  (MV)−1.2 [2]
Orbit [11]
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
Mass 8.50±0.53 [12]   M☉
Luminosity 3,754 [12]   L☉
Temperature 23,700 [12]   K
Rotation 0.901 d [13]
Rotational velocity (v sin i)165 [6]  km/s
B
Mass 4.5 [11]   M☉
Other designations
V1046 Orionis, BD−04°1183, HD 37017, HIP 26233, HR 1890, SAO 132317 [14]
Database references
SIMBAD data

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, [10] and is drifting further away with a radial velocity of +32 km/s. [9] The system is part of star cluster NGC 1981. [15]

The binary nature of this system was suggested by A. Blaauw and T. S. van Albada in 1963. [11] It is a double-lined [13] spectroscopic binary with an orbital period of 18.6556 days and an eccentricity of 0.31. [16] The eccentricity is considered unusually large for such a close system. [13] It has been suspected of being an eclipsing binary or rotating ellipsoidal variable, and the primary is also am SX Arietis variable. [8]

The primary is a helium-strong, magnetic chemically peculiar star [17] with a stellar classification of B1.5 Vp. [6] It has a magnetic field strength of 7,700  G , [18] and the helium concentrations are located at the magnetic poles. [19] V1046 Orionis was found to be a variable star by L. A. Balona in 1997, [13] and is now classified as an SX Arietis variable. [8] 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. [13] Radio emission has been detected that varies with the rotation period. [19]

The secondary component has an estimated 4.5 times the mass of the Sun. The class has been estimated as type B6III-IV. [13]

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.
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