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Title:
A New, Bright, Short-Period, Emission Line Binary in Ophiuchus
Authors:
Stark, M. A.; Wade, Richard A.; Thorstensen, John R.; Peters, Christopher S.; Smith, Horace A.; Miller, Robert D.; Green, E. M.
Affiliation:
AA(Department of Physics and Astronomy, University of Wyoming, Department 3905, 1000 E. University Ave., Laramie, WY 82071, USA ), AB(Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA ), AC(Department of Physics and Astronomy, 6127 Wilder Laboratory, Dartmouth College, Hanover, NH 03755-3528, USA), AD(Department of Physics and Astronomy, 6127 Wilder Laboratory, Dartmouth College, Hanover, NH 03755-3528, USA), AE(Department of Physics and Astronomy, Bio-Physical Sciences Bldg, Michigan State University, East Lansing, MI 48824-1116, USA), AF(Department of Physics and Astronomy, Bio-Physical Sciences Bldg, Michigan State University, East Lansing, MI 48824-1116, USA), AG(Steward Observatory, University of Arizona, Tucson, AZ 85721-0065, USA)
Publication:
The Astronomical Journal, Volume 135, Issue 3, pp. 991-999 (2008). (AJ Homepage)
Publication Date:
03/2008
Origin:
IOP
Astronomy Keywords:
binaries: close, novae, cataclysmic variables, stars: emission-line, Be, stars: individual: LS IV-08°3, stars: variables: other
DOI:
10.1088/0004-6256/135/3/991
Bibliographic Code:
2008AJ....135..991S

Abstract

The 11th magnitude star LS IV-08°3 has been classified previously as an OB star in the Luminous Stars survey, or alternatively as a hot subdwarf. It is actually a binary star. We present spectroscopy, spectroscopic orbital elements, and time-series photometry from observations made at the Kitt Peak National Observatory 2.1 m, Steward Observatory 2.3 m, MDM Observatory 1.3 m and 2.4 m, Hobby-Eberly 9.2 m, and Michigan State University 0.6 m telescopes. The star exhibits emission of varying strength in the cores of H and He I absorption lines. Emission is also present at 4686 Å (He II) and near 4640/4650 Å (N III/C III). Time-series spectroscopy collected from 2005 July to 2007 June shows coherent, periodic radial velocity variations of the Hα line, which we interpret as orbital motion with a period of 0.1952894(10) days. High-resolution spectra show that there are two emission components, one broad and one narrow, moving in antiphase, as might arise from an accretion disk and the irradiated face of the mass donor star. Less coherent, low-amplitude photometric variability is also present on a timescale similar to the orbital period. Diffuse interstellar bands indicate considerable reddening, which however is consistent with a distance of ~100-200 pc. The star is the likely counterpart of a weak ROSAT X-ray source, whose properties are consistent with accretion in a cataclysmic variable (CV) binary system. We classify LS IV-08°3 as a new member of the UX UMa subclass of CV stars.

Based in part on observations obtained with the Hobby-Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universität München, and Georg-August-Universität Göttingen.

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