EPSILON AURIGAE: AN IMPROVED SPECTROSCOPIC ORBITAL SOLUTION
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Stefanik-2010-EPSILON AURIGAE_ AN.pdf
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Author(s)
Stefanik, Robert P.
Torres, Guillermo
Lovegrove, Justin
Pera, Vivian E.
Latham, David W.
Zajac, Joseph
Mazeh, Tsevi
Date Issued
February 2010
Journal
The Astronomical Journal
Publisher
IOP Publishing
Citation
Stefanik, Robert P., Guillermo Torres, Justin Lovegrove, Vivian E. Pera, David W. Latham, Joseph Zajac, and Tsevi Mazeh. “EPSILON AURIGAE: AN IMPROVED SPECTROSCOPIC ORBITAL SOLUTION.” The Astronomical Journal 139, no. 3 (February 11, 2010): 1254–1260. doi:10.1088/0004-6256/139/3/1254.
Version
Final published version
Abstract
A rare eclipse of the mysterious object ε Aurigae will occur in 2009-2011. We report an updated single-lined spectroscopic solution for the orbit of the primary star based on 20 years of monitoring at the CfA, combined with historical velocity observations dating back to 1897. There are 518 new CfA observations obtained between 1989 and 2009. Two solutions are presented. One uses the velocities outside the eclipse phases together with mid-times of previous eclipses, from photometry dating back to 1842, which provide the strongest constraint on the ephemeris. This yields a period of 9896.0 ± 1.6 days (27.0938 ± 0.0044 years) with a velocity semi-amplitude of 13.84 ± 0.23 km s[superscript –1] and an eccentricity of 0.227 ± 0.011. The middle of the current ongoing eclipse predicted by this combined fit is JD 2,455,413.8 ± 4.8, corresponding to 2010 August 5. If we use only the radial velocities, we find that the predicted middle of the current eclipse is nine months earlier. This would imply that the gravitating companion is not the same as the eclipsing object. Alternatively, the purely spectroscopic solution may be biased by perturbations in the velocities due to the short-period oscillations of the supergiant.
MIT Department
Lincoln Laboratory
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DOI of Published Version
https://doi.org/10.1088/0004-6256/139/3/1254
