Photospheric Line-profile Variability From Tidal Interactions

Details Photospheric Line-profile Variability From Tidal Interactions Photospheric Line-profile Variability From Tidal Interactions

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.0328k&link_type=abstract

American Astronomical Society, AAS Meeting #211, #03.28; Bulletin of the American Astronomical Society, Vol. 39, p.727

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We have developed a code that performs an ``ab initio" calculation of the distortions produced by tidal interactions in the photospheric absorption line profiles. The computation begins by solving the equations of motion of small surface elements in a thin outer shell of the star. The forces that are included are the gravitational forces of both stars, the centrifugal, coriolis and viscous forces, and forces due to gas pressure. The resultant velocity field over the stellar surface is then used to compute the absorption line profiles in the frame of reference of the observer. The line-profile variability that is predicted by the code includes the presence of narrow peaks and troughs that propagate from the blue to the red wing of the absorption line, similar to features that are observed in many binary systems. We will present the results of our calculations for the B1 III-IV star in Spica (P=4.01 d, e=0.146), and for the K-star component in V471 Tau (P=0.521 h, e=0), under the assumption that its stellar rotation period differs slightly from the orbital period. We will speculate on some of the additional observational effects that may be produced by the tidal interactions.

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