The state of ionization in nova shells. II - Integration of the ionization equation for optically thick shells

Astronomy and Astrophysics – Astrophysics

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Gas Ionization, Light Curve, Novae, Numerical Integration, Optical Thickness, Stellar Envelopes, Astronomical Models, Hydrogen Ions, Lyman Spectra, Stellar Radiation

Scientific paper

The ionization equation for an expanding spherically symmetric homogeneous hydrogen shell surrounding a central star is integrated over time to investigate a possible explanation for the light curves of novae which show a marked minimum, such as that of DQ Herculis 1934. Considerations are discussed which restrict the integration to optically thick shells, particularly the assumption that all photons arising from recombinations of protons and electrons to hydrogen atoms in the ground state are reabsorbed, ionizing other hydrogen atoms. The output of visible radiation between 5400 and 5500 A is calculated from the resulting dependence of the degree of ionization on time and position in the shell, and 'light curves' are derived for a number of shells in which the mass, electron temperature, initial radius, and expansion velocity are varied. It is suggested that the assumed absorption process will continue in the outer shell layers as the shell expands, but will cease when the whole shell has become completely ionized, resulting in a decrease in the visual brightness of the shell.

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