Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003astl...29..775f&link_type=abstract
Astronomy Letters, vol. 29, p. 775-782 (2003)
Astronomy and Astrophysics
Astronomy
Scientific paper
Based on a self-consistent solution of the equations of gas dynamics, kinetics of hydrogen atomic level populations, and radiative transfer, we analyze the structure of a shock wave that propagates in a partially ionized hydrogen gas. We consider the radiative transfer at the frequencies of spectral lines by taking into account the effects of a moving medium in the observer's frame of reference. The flux in Balmer lines is shown to be formed behind the shock discontinuity at the initial hydrogen recombination stage. The Doppler shift of the emission-line profile is approximately one and a half times smaller than the gas flow velocity in the Balmer emission region, because the radiation field of the shock wave is anisotropic. At Mach numbers M_1 < 10 and unperturbed gas densities rho_1 = 10^{-10} g/cm^3, the Doppler shift is approximately one third of the shock velocity U_1. The FWHM of the emission-line profile is related to the shock velocity by delta_phi = k_phi U_1, where k_phi = 1, 0.6, and 0.65 for the H_alpha, H_beta, and H_gamma lines, respectively.
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