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Nonlinear Radial Pulsations for Hot 20-M⊙ Models

Published online by Cambridge University Press:  12 April 2016

Benjamin A. Austin ,
Joyce A. Guzik ,
Kate M. Despain  and
Matthew R. Templeton
Benjamin A. Austin
Affiliation:
Los Alamos National Laboratory, X-2, MS T085, Los Alamos, NM 87545-2345, USA
Joyce A. Guzik
Affiliation:
Los Alamos National Laboratory, X-2, MS T085, Los Alamos, NM 87545-2345, USA
Kate M. Despain
Affiliation:
Los Alamos National Laboratory, X-2, MS T085, Los Alamos, NM 87545-2345, USA
Matthew R. Templeton
Affiliation:
American Association of Variable Star Observers, 25 Birch St., Cambridge, MA 02138, USA

Abstract

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We present the results of calculations that predict a radial pulsation instability region for hot 20-M⊙ stars within a narrow band around Teff = 22,000 K. These models have exhausted core hydrogen and are undergoing shell hydrogen burning, and have luminosities similar to the most massive β Cephei stars, but are slightly cooler and more evolved. The pulsations grow to a radial velocity amplitude of ~20 km s-1with a period of ~0.75 d. The amplitude increases for higher Z and lower Y models.

Information

Type
Part 8. New theoretical developments in stellar pulsation and variability
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 453 - 457
Copyright
Copyright © Astronomical Society of the Pacific 2004

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