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]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas[9] |
| Distance | 1,230 ± 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 | |
| Mass | 8.50±0.53[3] M☉ |
| Luminosity | 3,754[3] L☉ |
| Temperature | 23,700[3] K |
| Rotation | 0.901 d[11] |
| Rotational velocity (v sin i) | 165[5] km/s |
| B | |
| Mass | 4.5[10] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
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
edit- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ a b 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.
- ^ a b c d e 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.
- ^ Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
- ^ a b c 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.
- ^ a b 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.
- ^ a b c 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.
- ^ a b 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.
- ^ a b c d 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.
- ^ a b c 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.
- ^ a b c d e f 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.
- ^ "V1046 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-31.
- ^ 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.
- ^ 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, A26.
- ^ 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.
- ^ 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.
- ^ a b 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.