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OP versus OPAL opacities: consequences for B star oscillations

Published online by Cambridge University Press:  26 May 2016

A.A. Pamyatnykh ,
W.A. Dziembowski ,
P. Moskalik  and
M.J. Seaton
A.A. Pamyatnykh
Affiliation:
N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland Institute of Astronomy, 48 Pyatnitskaya St., 109017 Moscow, Russia
W.A. Dziembowski
Affiliation:
N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
P. Moskalik
Affiliation:
N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
M.J. Seaton
Affiliation:
Department of Physics and Astronomy, University College London, Gower St., London WC1E 6BT, UK

Extract

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Radiative Rosseland-mean opacities for stellar envelopes from The Opacity Project, hereafter OP, became available (Seaton et al. 1993). Here we present a preliminary survey of pulsation properties of B-star models, obtained with this new opacity data and compare these properties with those of models built with the OPAL opacities (Iglesias, Rogers and Wilson 1992). The two opacity projects employ very different approximations in treatment of the plasma and atomic physics. In addition the OP tables are calculated including absorbtion due to three iron group elements ignored in OPAL tables, namely Cr, Mn and Ni.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 70 - 72
Copyright
Copyright © Kluwer 1994 

References

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