Hydrodynamic Interactions Between Massive Stars and Their Environments

Details Hydrodynamic Interactions Between Massive Stars and Their Environments Hydrodynamic Interactions Between Massive Stars and Their Environments

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997cokon.100..239d&link_type=abstract

Communications of the Konkoly Observatory, No. 100 (Vol. XII, 2), p. 239-252 (1997)

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It is becoming clear that a proper treatment of the interaction of stars with their environment must take into account the inhomogeneous nature of circumstellar material. Our ongoing study of this problem is revealing a rich variety of physical effects that have important implications for star-forming regions and the diffuse sources found within them. We describe the mechanisms by which mass is lost from dense clumps and formed into tails which have a range of lengths and shapes depending on the flow conditions. These considerations are applied to a model for ultracompact Hii regions (UCHIIR) in which, as a result of mass injection, the ionization front that is normally expected around a HII region is replaced by a recombination front. The regions can reach a steady equilibrium, avoiding the well known lifetime problem for UCHIIR models. In another example, properties of the Wolf-Rayet nebula RCW 58 are explained by a mass-loaded model.

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