Astronomy:HD 37017

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Short description: Binary star system in the constellation Orion
HD 37017
V1046OriLightCurve.png
A light curve for V1046 Orionis, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Orion
Right ascension  05h 35m 21.86770s[2]
Declination −04° 29′ 39.0409″[2]
Apparent magnitude (V) 6.553[3]
Characteristics
Evolutionary stage B2/3V[4] (B1.5 Vp He strong[5])
U−B color index −0.79[6]
B−V color index −0.14[6]
Variable type SX Ari[7]
Astrometry
Radial velocity (Rv)+32±2[8] km/s
Proper motion (μ) RA: 1.88±0.09[9] mas/yr
Dec.: 1.20±0.14[9] mas/yr
Parallax (π)2.643 ± 0.075[9] mas
Distance1,230 ± 40 ly
(380 ± 10 pc)
Orbit[10]
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[3] M☉
Luminosity3,754[3] L☉
Temperature23,700[3] K
Rotation0.901 d[11]
Rotational velocity (v sin i)165[5] km/s
B
Mass4.5[10] M☉
Other designations
V1046 Orionis, BD−04°1183, HD 37017, HIP 26233, HR 1890, SAO 132317[12]
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 6.55.[3] It is located at a distance of approximately 1,230 light years based on parallax,[9] and is drifting further away with a radial velocity of +32 km/s.[8] The system is part of star cluster NGC 1981.[13]

The binary nature of this system was suggested by A. Blaauw and T. S. van Albada in 1963.[10] It is a double-lined[11] spectroscopic binary with an orbital period of 18.6556 days and an eccentricity of 0.31.[14] The eccentricity is considered unusually large for such a close system.[11] It forms a suspected eclipsing binary that ranges in brightness from 6.54 down to 6.58.[7]

The primary is a helium-strong, magnetic chemically peculiar star[15] with a stellar classification of B1.5 Vp.[5] It has a magnetic field strength of 7,700 G,[16] and the helium concentrations are located at the magnetic poles.[17] V1046 Orionis was found to be a variable star by L. A. Balona in 1997,[11] and is now classified as an SX Arietis variable.[7] 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.[11] Radio emission has been detected that varies with the rotation period.[17]

The secondary component has an estimated 4.5 times the mass of the Sun. The class has been estimated as type B6III-IV.[11]

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  2. ↑ 2.0 2.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 3.3 3.4 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, doi:10.1002/asna.200911355, Bibcode: 2010AN....331..349H. 
  4. ↑ 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. ↑ 5.0 5.1 5.2 Abt, Helmut A. et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, doi:10.1086/340590, Bibcode: 2002ApJ...573..359A. 
  6. ↑ 6.0 6.1 Walker, M. F. (February 1969), "Studies of extremely young clusters. V. Stars in the vicinity of the Orion nebula", Astrophysical Journal 155: 447, doi:10.1086/149881, Bibcode: 1969ApJ...155..447W. 
  7. ↑ 7.0 7.1 7.2 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S. 
  8. ↑ 8.0 8.1 Blaauw, A. et al. (April 1963), "Radial Velocities of B-Type Stars in the Nearest Associations.", Astrophysical Journal 137: 791, doi:10.1086/147556, Bibcode: 1963ApJ...137..791B. 
  9. ↑ 9.0 9.1 9.2 9.3 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, doi:10.3847/1538-4357/834/2/142, Bibcode: 2017ApJ...834..142K. 
  10. ↑ 10.0 10.1 10.2 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. 
  11. ↑ 11.0 11.1 11.2 11.3 11.4 11.5 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. 
  12. ↑ "V1046 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V1046+Ori. 
  13. ↑ 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, doi:10.1111/j.1365-2966.2010.17034.x, Bibcode: 2010MNRAS.407.1875M. 
  14. ↑ Ducati, J. R. et al. (January 2011), "The mass ratio and initial mass functions in spectroscopic binaries", Astronomy and Astrophysics 525: 9, doi:10.1051/0004-6361/200913895, A26, Bibcode: 2011A&A...525A..26D, http://www.lume.ufrgs.br/bitstream/10183/99264/1/000821103.pdf. 
  15. ↑ 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, doi:10.1093/mnras/stz1678, Bibcode: 2019MNRAS.487.5922G. 
  16. ↑ 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, doi:10.1051/0004-6361:20040060, Bibcode: 2004A&A...418..593T. 
  17. ↑ 17.0 17.1 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 (San Francisco: Astronomical Society of the Pacific) 44 (138): p. 541, Bibcode: 1993ASPC...44..541L. 

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