Theoretical emission line profiles for novae

This paper discusses theoretical emission line profiles that were computed for spherically symmetric, nonrotating, radially expanding models of shells ejected by novae. The theory of the formation of the emission line profile is developed using Gaussian wavelength distributions for the volume absorption and emission coefficients. The expression for the energy emission from the shell is evaluated in detail using numerical integration techniques. The behavior of the theoretical profiles is examined for changes in the following parameters: distribution through the shell of the speed of expansion; thermal broadening; and excitation conditions, specified by the distributions of the densities of absorbing and emitting atoms. An analysis is made of the regions of the shell that contribute to different parts of the profiles. The analysis of the behavior of the theoretical profiles is used to find a model to fit observations of Hepsilon and [OIII], lambda4363, of Nova Herculis 1963 on June 14, 1963. (Diss. Abstr. Int., B)