HD 37017
Binary star system in the constellation Orion
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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]