Deconstructing HD 28867
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.
Keywords
Cite
@article{arxiv.astro-ph/0301003,
title = {Deconstructing HD 28867},
author = {Frederick M. Walter and Tracy L. Beck and Jon A. Morse and Scott J. Wolk},
journal= {arXiv preprint arXiv:astro-ph/0301003},
year = {2009}
}
Comments
accepted by the Astronomical Journal