Deconstructing HD 28867

Frederick M. Walter; Tracy L. Beck; Jon A. Morse; Scott J. Wolk

doi:10.1086/368245

Deconstructing HD 28867

Frederick M. Walter
, Tracy L. Beck
, Jon A. Morse
, Scott J. Wolk

Physics and Astronomy

Gemini Observatory
University of Colorado Boulder
Harvard-Smithsonian Ctr. Astrophys.

Research output: Contribution to journal › Article › peer-review

12 Scopus citations

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 multiwavelength 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 μm, it and the B9 star are equally bright. We see evidence of radial velocity variability in the cool component of over 34 km s^-1. 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.

Original language	English
Pages (from-to)	2123-2133
Number of pages	11
Journal	Astronomical Journal
Volume	125
Issue number	4 1768
DOIs	https://doi.org/10.1086/368245
State	Published - Apr 2003

Keywords

Open clusters and associations: individual (Taurus-Auriga)
Stars: individual (HD 28867)

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10.1086/368245

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title = "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 multiwavelength 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 μm, it and the B9 star are equally bright. We see evidence of radial velocity variability in the cool component of over 34 km s-1. 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 = "Open clusters and associations: individual (Taurus-Auriga), Stars: individual (HD 28867)",

author = "Walter, \{Frederick M.\} and Beck, \{Tracy L.\} and Morse, \{Jon A.\} and Wolk, \{Scott J.\}",

year = "2003",

month = apr,

doi = "10.1086/368245",

language = "English",

volume = "125",

pages = "2123--2133",

journal = "Astronomical Journal",

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TY - JOUR

T1 - Deconstructing HD 28867

AU - Walter, Frederick M.

AU - Beck, Tracy L.

AU - Morse, Jon A.

AU - Wolk, Scott J.

PY - 2003/4

Y1 - 2003/4

N2 - 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 multiwavelength 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 μm, it and the B9 star are equally bright. We see evidence of radial velocity variability in the cool component of over 34 km s-1. 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.

AB - 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 multiwavelength 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 μm, it and the B9 star are equally bright. We see evidence of radial velocity variability in the cool component of over 34 km s-1. 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.

KW - Open clusters and associations: individual (Taurus-Auriga)

KW - Stars: individual (HD 28867)

UR - https://www.scopus.com/pages/publications/0042761952

U2 - 10.1086/368245

DO - 10.1086/368245

M3 - Article

AN - SCOPUS:0042761952

SN - 0004-6256

VL - 125

SP - 2123

EP - 2133

JO - Astronomical Journal

JF - Astronomical Journal

IS - 4 1768

ER -

Deconstructing HD 28867

Abstract

Keywords

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