Interstellar bubbles. II - Structure and evolution
R. Weaver, R. McCray, J. Castor, P. Shapiro, R. Moore;
ApJ, 1977, 218, 377
ABSTRACT:The detailed structure of the interaction of a strong stellar wind with the interstellar medium is presented.
First, an adiabatic similarity
solution is given which is applicable at early times.
Second, a similarity
solution is derived which includes the effects of thermal conduction between
the hot (about 1 million K) interior and the cold shell of swept-up
interstellar matter.
This solution is then modified to include the effects of
radiative energy losses.
The evolution of an interstellar bubble is
calculated, including the radiative losses.
The quantitative results for the
outer-shell radius and velocity and the column density of highly ionized species
such as O VI are within a factor 2 of the approximate results of Castor,
McCray, and Weaver (1975).
The effect of stellar motion on the structure of a
bubble, the hydrodynamic stability of the outer shell, and the observable
properties of the hot region and the outer shell are discussed.
KEYWORDS: interstellar gas, plasma interactions, stellar winds, adiabatic flow, bubbles, conductive heat transfer, early stars, energy dissipation, hydrodynamics, ion density (concentration), radiative transfer, stellar motions
CODE: weaver77