Deconstructing HD 28867 | Zendy

F. M. Walter | Zendy; Tracy L. Beck | Zendy; Jon A. Morse | Zendy; S. J. Wolk | Zendy

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Deconstructing HD 28867

Author(s) -

F. M. Walter,

Tracy L. Beck,

Jon A. Morse,

S. J. Wolk

Publication year - 2003

Publication title -

the astronomical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.61

H-Index - 271

eISSN - 1538-3881

pISSN - 0004-6256

DOI - 10.1086/368245

Subject(s) - physics , astrophysics , stars , star (game theory) , astronomy , radial velocity , a type main sequence star

The 3" pair of B9 stars, HD 28867, is one of the brightest X-ray sources inthe Taurus-Auriga star forming region. In this multi-wavelength study, weattempt to deduce the source of the X-ray emission. We show that the Eastcomponent is the X-ray source. The East component has a near-IR excess anddisplays narrow absorption lines in the optical, both of which are consistentwith a cool stellar companion. This companion is one of the brightest low masspre-main sequence stars in Tau-Aur; at 2 microns it and the B9 star are equallybright. We see evidence for radial velocity variability in the cool componentof >34 km/s. It is not visible in K band speckle imaging, which constrains thecompanion to lie within 14 AU of the B star. We also report on a possible fourth member of the group, an M1 star 18" southof HD 28867.Comment: accepted by the Astronomical Journa

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