Physics
Scientific paper
Mar 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220.1024k&link_type=abstract
Astrophysical Journal, Part 1, vol. 220, Mar. 15, 1978, p. 1024-1040.
Physics
20
Energy Transfer, Plasma Dynamics, Radiative Transfer, Shock Waves, Stellar Atmospheres, Astronomical Models, Atmospheric Physics, Balmer Series, Elastic Waves, Energy Levels, Thermodynamic Equilibrium, Wave Propagation
Scientific paper
The interaction between radiation and a shock wave propagating through a stellar atmosphere is investigated. Departures from local thermodynamic equilibrium (LTE) are permitted in the first two levels of a 10-level hydrogen atom; levels 3-10 are in LTE. A piston moving at constant velocity into the bottom of the atmosphere drives a shock wave. This shock produces precursor radiation that diffuses through the gas well ahead of the shock and causes a mild luminosity flash in the emergent Balmer and free-free radiation when it reaches the surface. The precursor wave deposits a large amount of radiative energy in the outer layers of the atmosphere, initiating a radiation-induced pressure wave. The process of energy transfer from the radiation field to the compression wave is similar to the Eddington valve mechanism which drives stellar pulsations. Material is accelerated outward by the radiation-induced wave; eventually it free-falls inward, hits the quasistationary atmosphere, and forms an accretion shock. The piston driven shock is weakened by radiative energy losses. When it reaches the surface, the shock is invisible in the continuum radiation.
Kalkofen Wolfgang
Klein Richard I.
Stein Robert F.
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