Abstract
Consideration is given to the role of ionization fronts and associated effects in the expansion of a planetary nebula formed by the collision of a high-velocity stellar wind with an expanding H II region. A similarity transformation is used to obtain solutions to the dynamic and radiative equations in the propagation of an ionization front, possibly preceded by a shock wave, in gas representing the remnant of a slow stellar wind. Three different types of flow configurations are obtained for the case of an ambient gas density decreasing as the square of the radius, corresponding to weak R, weak D and strong D ionization fronts. All types of flow configurations are found to be characterized by a positive velocity gradient within the high-density, swept-up shell of ionized gas formed ahead of the contact discontinuity. In contrast to previous models of nebular expansion, the present solutions exhibit flow structure within the ionized gas and the presence of long-lived shocks.
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