Astron. Astrophys. 337, 183-197 (1998)

HD 37017 = V 1046 Ori. A double-lined spectroscopic binary with a B2e He-strong magnetic primary ^*

C.T. Bolton ^{** 1}, P. Harmanec ², R.W. Lyons ^{1, 3}, A.P. Odell ^{*** 4} and Diane M. Pyper <sup>5

1</sup> David Dunlap Observatory, University of Toronto, P.O. Box 360, Richmond Hill, ON, L4C 4Y6 Canada (bolton@struve.astro.utoronto.ca)
² Astronomický ústav Akademie v d eské republiky, 251 65 Ond ejov, Czech Republic (hec@sunstel.asu.cas.cz)
³ Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093-0424, USA (rlyons@ucsd.edu)
⁴ Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86011, USA (Andy.Odell@nau.edu)
⁵ Physics Dept., University of Nevada Las Vegas, Las Vegas, NV 89154, USA (dpsmith@nevada.edu

Received 4 March 1998 / Accepted 5 June 1998

Abstract

We report on a detailed spectroscopic and photometric study of V1046 Orionis undertaken to resolve uncertainties about the period(s) and causes of the spectroscopic and photometric variations of this helium-strong star. We have detected the lines of the secondary star in an extensive series of photographic and electronic spectra. This eliminates any doubt about the duplicity of this star. The orbital elements we derive from our measures of these spectra confirm the unusually large orbital eccentricity, e = 0.433, for the short, P = 18.65612, orbital period. The line profiles, V/R ratio of the double H emission, residuals of the primary radial velocities from the orbital velocity curve, brightness and colour of the object, magnetic field, and radio emission of this system all vary with a period of 0.9011836. We tentatively follow earlier investigators in interpreting this as the rotational period of the primary and summarize the evidence of the phase shifts among the different phenomena, using the accurate value of the 0.9 period, to put tight constraints on any future model of these changes. We postpone our own attempt at a quantitative modelling of the variations with the 0.9 period for a separate study.

Key words: stars: binaries: spectroscopic stars: fundamental parameters stars: oscillations stars: individual: V 1046 Ori

* Tables 3 and 5 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html
** Visiting Astronomer, Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique of France, and the University of Hawaii.
*** Visiting astronomer, Kitt Peak National Observatory, National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.

Send offprint requests to: C.T. Bolton

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Contents

• 1. Introduction
• 2. Observations and reductions
  • 2.1. Spectroscopy
  • 2.2. Photometry
• 3. Period analysis
  • 3.1. Radial velocities
  • 3.2. Photometry
• 4. Final spectroscopic orbital elements
• 5. Basic physical properties of the system
  • 5.1. Phase relations among the short-period variations
  • 5.2. Basic physical properties of the primary
  • 5.3. Dimensions of the binary system
  • 5.4. Estimated properties of the secondary star
• 6. Rapid variations of the primary
• 7. Puzzles?
• Acknowledgements
• References

© European Southern Observatory (ESO) 1998

Online publication: August 6, 1998
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