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Pulsation Hydrodynamics of Luminous Blue Variables and Pulsation-Driven Winds

Published online by Cambridge University Press:  12 April 2016

Joyce A. Guzik ,
Arthur N. Cox ,
Kate M. Despain  and
Michael S. Soukup
Joyce A. Guzik
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM 87545-2345USA
Arthur N. Cox
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM 87545-2345USA
Kate M. Despain
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM 87545-2345USA
Michael S. Soukup
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM 87545-2345USA

Abstract

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Many physical factors, including radial and nonradial pulsation, rotation, radiation pressure, convection, magnetic fields, or dynamical instabilities may play important roles in the hydrodynamics of Luminous Blue Variables. We review the current status of hydrodynamic modeling of LBV envelopes, and describe results of our models using the one-dimensional nonlinear hydrodynamics code of Ostlie and Cox. We find that the models pulsate in several simultaneous radial modes, driven by the helium and Fe ionization к effect. The pulsations have quasi-periods between 5 and 80 days, with radial velocity amplitudes of 50-200 km/sec, and may be identified with the LBV microvariations. In some cases, depending on luminosity-to-mass ratio and helium abundance, deep layers in the model can periodically exceed the Eddington luminosity limit. The key to exceeding LE is the inclusion of the time dependence of convection: Near the regions of opacity peaks produced by Fe and helium ionization, convection is turning on and off during each pulsation cycle. If convection cannot turn on rapidly enough to transport the required luminosity through the region, the Eddington limit is exceeded. If this region of the star is sufficiently adiabatic, an “outburst” may occur. In the hydrodynamic models, an outburst is indicated by the photospheric radial velocity suddenly becoming very large, and the photospheric radius increasing monotonically over several pulsation cycles. Such pulsation-triggered outbursts may be responsible for the driving of variable, nonspherical winds. If large and infrequent enough, these outbursts may be identified with the classic LBV eruptions accompanied by episodic mass loss.

Type
Section V Pulsation
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 337 - 344
Copyright
Copyright © Springer-Verlag 1999

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