Computer Science – Numerical Analysis
Scientific paper
Sep 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1171..353k&link_type=abstract
RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND RADIATION HYDRODYNAMICS: Proceedings of the International Confe
Computer Science
Numerical Analysis
Binary Stars, Stellar Atmospheres, Numerical Analysis, Binary And Multiple Stars, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, Numerical Approximation And Analysis
Scientific paper
Binary stars in eccentric orbits are the clearest example of stars whose equatorial rotation velocity is not synchronized with orbital motion. Under these conditions, the surface velocity field is perturbed from its purely rotational nature, thus modifying the shape of the observationally-detectable photospheric absorption lines on a variety of timescales. Absorption lines are used to derive basic stellar parameters and gain a better physical understanding of the star. Although their variability is often interpreted in terms of non-radial pulsation theory, it is important to understand the nature of the surface velocity fields that are induced by the tidal interactions alone, especially under conditions of rapid rotation and large orbital eccentricity, where the perturbations become highly non-linear.
We use a time-marching numerical calculation from first principles to model the surface velocity field due to the tidal interaction (Moreno & Koenigsberger 1999; Toledano et al. 2007). This velocity field is then projected along the line-of-sight to the observer to predict the orbital phase-dependent line-profile variability (Moreno et al. 2005). We compare our model results with very high quality observational data of the B-type binary system α Vir (Spica, HD 116658, P = 4d, e = 0.1), whose variability has in the past been modeled in the context of non-radial pulsations (Smith 1985). Our model reproduces the general features of the observations (Harrington et al. 2009). It is interesting to note that because tidal flows are associated with viscous shear energy dissipation, the question arises as to whether the atmospheric structure of an asynchronously rotating binary star may be reliably modeled using techniques that disregard the dynamical effects on the stellar surface of the tidal interactions.
Harrington David
Koenigsberger Gloria
Moreno Edmundo
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