Structure and energy transfer of unstable hot star winds

Details Structure and energy transfer of unstable hot star winds Structure and energy transfer of unstable hot star winds

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.221..393f&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 221, no. 1-2, p. 393-408

Statistics

Computation

Computational Astrophysics, Energy Transfer, Hot Stars, Hydrodynamics, Stability, Stellar Physics, Stellar Structure, Stellar Winds, Euler Equations Of Motion, Nonlinearity, Perturbation, Shock Waves, Stellar Models, Time Dependence

Scientific paper

Due to the instability of the radiation line force, the winds of hot, luminous stars should show a pronounced time-dependence resulting from the nonlinear growth of initially small perturbations. We describe the time-dependent wind structure obtained with an independently developed code. We find that the response of the wind to periodic base perturbations remains largely periodic, at least up to r approximately equals 2...3 R*, with no clear evidence of stochastic behavior. In order to test the foregoing assumption of isothermality and to compute the X-ray emission from models of structured winds, we have also incorporated the energy equation into our simulations. We encountered the numerical problem that all radiative cooling zones collapse because of the oscillatory thermal instability . We present a method to hinder this collapse by changing the cooling function at low temperatures. The resulting wind shows resolved cooling zones; but, for a supergiant wind relatively close to the star (r approximately less than 10 R*), the marcroscopic wind structure is very similar to isothermal calculations.

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