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Nonlinear hydrodynamic simulations of radial pulsations in massive stars

Published online by Cambridge University Press:  18 February 2014

Catherine Lovekin
Affiliation:
Department of Physics, Mount Allison University 67 York St., Sackville, NB E4L 1E6Canada email: [email protected] Los Alamos National Laboratory XTD-NTA, MS T086, Los Alamos, NM 87545USA email: [email protected]
Joyce A. Guzik
Affiliation:
Los Alamos National Laboratory XTD-NTA, MS T086, Los Alamos, NM 87545USA email: [email protected]
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Abstract

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We investigate the radial pulsation properties of massive main-sequence stars using both linear and non-linear calculations. Using 20, 40, 60 and 85 solar-mass models evolved by Meynet et al. (1994), we calculate nonlinear hydrodynamic envelope models including the effects of time-dependent convection. Many of these models are massive enough to lose a significant amount of mass as they evolve, which also reveals more helium-rich layers. This allows us to investigate the dependence of pulsation on mass, metallicity and surface helium abundance. We find that as a model loses mass, the periods become longer relative to the period predicted by the period-mean density relation (period × $\sqrt{\overline{\rho}}$ is proportional to a constant, Q) for the initial model. Increased surface helium abundance causes a dramatic decrease in the period relative to that expected from Q, while changing the metallicity had little impact on the expected periods.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2014 

References

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