Deconstructing HD 28867
arXiv:astro-ph/0301003 · doi:10.1086/368245
Abstract
The 3" pair of B9 stars, HD 28867, is one of the brightest X-ray sources in the Taurus-Auriga star forming region. In this multi-wavelength study, we attempt to deduce the source of the X-ray emission. We show that the East component is the X-ray source. The East component has a near-IR excess and displays narrow absorption lines in the optical, both of which are consistent with a cool stellar companion. This companion is one of the brightest low mass pre-main sequence stars in Tau-Aur; at 2 microns it and the B9 star are equally bright. We see evidence for radial velocity variability in the cool component of >34 km/s. It is not visible in K band speckle imaging, which constrains the companion to lie within 14 AU of the B star. We also report on a possible fourth member of the group, an M1 star 18" south of HD 28867.
accepted by the Astronomical Journal
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- Gaia EDR3 Reveals the Substructure and Complicated Star Formation History of the Greater Taurus-Auriga Star Forming Complex
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- B- and A-Type Stars in the Taurus-Auriga Star Forming Region
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