THE EXPANSION OF A STELLAR WIND BUBBLE WITHIN A NON-SINGULAR, STRATIFIED CORE
We study analytically the expansion of a non-radiative bubble (driven by the wind from a massive star) into an environment with a non-singular, self-gravitating isothermal sphere density stratification. We derive the equation of motion forthe outer radius of the bubble (using the assumptions of the...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2012 |
| País: | México |
| Institución: | Universidad Nacional Autónoma de México |
| Repositorio: | Redalyc-UNAM |
| OAI Identifier: | oai:redalyc.org:57124423007 |
| Acceso en línea: | https://www.redalyc.org/articulo.oa?id=57124423007 |
| Access Level: | acceso abierto |
| Palabra clave: | Física, Astronomía y Matemáticas ISM: evolution stars: formation ISM: kinematics and dynamics |
| Sumario: | We study analytically the expansion of a non-radiative bubble (driven by the wind from a massive star) into an environment with a non-singular, self-gravitating isothermal sphere density stratification. We derive the equation of motion forthe outer radius of the bubble (using the assumptions of the classical analytic model for expanding bubbles, but allowing the outer shock to have the appropri- ate strong/weak shock transition). The model equation has a single dimensionlessparameter that determines whether or not the outer shock becomes weak. We find that O star bubbles within dense, stratified molecular cloud cores (possibly associ-ated with some of the observed ultracompact HII regions) are in the "strong shock" limit. |
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