Deconstructing HD 28867

Details Deconstructing HD 28867 Deconstructing HD 28867

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.9313w&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #93.13; Bulletin of the American Astronomical Society, Vol. 34, p.1260

Astronomy and Astrophysics

Astronomy

Scientific paper

The 3\arcsec pair of B9 stars, HD 28867, is one of the brightest X-ray sources in the Taurus-Auriga star forming region. 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 mid-K spectral type 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. It is not a radial velocity variable, and is not separable in K band speckle imaging, which constrains the K star to lie within 30 AU of the B star. We also report on a possible fourth member of the group, an early M star 18\arcsec south of HD 28867.

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