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M. V. McSwain (GSU)
HD~16429 is a triple star system with a single-line spectroscopic binary and a widely separated third component, previously identified via speckle interferometry. For the first time, the spectral contributions of the two visible components have been isolated using a Doppler tomography algorithm, but unfortunately the spectroscopic secondary is too faint and remains hidden. The unseen star is probably not a compact companion, but rather a less luminous star whose signature is overwhelmed by its close, brighter companion. This poster presents the orbital elements for the unblended spectroscopic binary as well as estimates of the spectral types and relative flux contributions for each visible component. Due to its light curve variability, this star has previously been classified as a \beta Cephei variable, a class of stars with non-radial pulsations. However, using its Hipparcos light curve, this classification has been found to be inaccurate, and the variability is instead attributed to variable stellar winds from the single, speckle component of the system. The environment around HD~16429, including the nearby Be X-ray binary LSI~+61~103, is also examined.
Institutional support has been provided from the GSU College of Arts and Sciences and from the Research Program Enhancement fund of the Board of Regents of the University System of Georgia, administered through the GSU Office of the Vice President for Research and Sponsored Programs.
The author(s) of this abstract have provided an email address for comments about the abstract: mcswain@chara.gsu.edu
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Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.