The structure of shocks in the atmospheres of pulsating stars

摘要: The structure of shocks propagating through partially ionized hydrogen gas with characteristics typical the atmospheres RR Lyr, W Vir, and RV Tau type variables is analyzed in terms a self-consistent solution equations dynamics, atomic kinetics, radiation transfer. solutions were obtained for shock waves velocities 20 km/s≤U1≤90 km/s unperturbed temperatures 3000 K≤T1≤9000 K density ρ1=10−10 g/cm3. fraction energy gas-dynamic flux converted into increases amplitude, ratio emitted by to kinetic 0.4≲ℜ≲0.8 U1 considered. This also slightly ambient temperature T1 due an increase ionization radiative precursor. leading edge opposite flow several percent higher than direction trailing shock. Radiation mostly concentrated Balmer continuum, region efficient Lyman transfer includes layers located near viscous jump (δX=±104 cm). final gas-compression units limiting compression corresponding isothermal approximation virtually independent from r≈0.5 at T1=3000 r≈0.9 T1=9000 K.