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An empirical pipeline for determining the viscosity parameter for Be star disks

Published online by Cambridge University Press:  23 January 2015

Leandro R. Rímulo ,
Alex C. Carciofi ,
Thomas Rivinius  and
Xavier Haubois
Leandro R. Rímulo
Affiliation:
University of São Paulo, Dept. of Astronomy, Brazil email: lrrimulo@usp.br
Alex C. Carciofi
Affiliation:
University of São Paulo, Dept. of Astronomy, Brazil email: lrrimulo@usp.br
Thomas Rivinius
Affiliation:
ESO, Chile
Xavier Haubois
Affiliation:
LESIA, Observatoire de Paris, France
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Abstract

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Be star phenomenology is strongly associated with their viscous circumstellar disks. Recently, models became available for the temporal evolution of these disks when subject to variable mass ejection rates. In this contribution we will discuss how these dynamical disk models, modeled with the radiative transfer code HDUST, can be used for constraining fundamental disk parameters, such as the α viscosity parameter, and we will report on an ongoing effort to model light curves of a large number of stars.

Keywords

hydrodynamicsradiative transfertechniques: photometricstars: mass loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 133 - 134
Copyright
Copyright © International Astronomical Union 2015 

References

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