The structure and evolution of interstellar bubbles in a multiphase interstellar medium. I - Physical model

Details The structure and evolution of interstellar bubbles in a multiphase interstellar medium. I - Physical model The structure and evolution of interstellar bubbles in a multiphase interstellar medium. I - Physical model

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.224..701w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 224, Feb. 1, 1987, p. 701-720.

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Computation

9

Astronomical Models, Computational Astrophysics, Interstellar Gas, Stellar Winds, Hydrodynamics, Hydrogen Clouds, Oort Cloud, Photoionization, Supernova Remnants

Scientific paper

A method for modeling the structure of interstellar bubbles in a multiphase interstellar medium is presented. The computational scheme involves modeling both the intercloud fluid (ICF) and the clouds on separate numerical grids. The standard hydrodynamic equations must be modified to include effects of mass, momentum, and energy exchange between the ICF and the clouds. These exchange processes come about principally because Lyman continuum radiation from the central star ionizes the cold clouds, providing a large source of mass injection to the ICF. A less significant source of mass exchange is thermal evaporation of clouds due to hot gas in the bubble interior. The cloud motions caused both by drag against the ICF and by the Oort-Spitzer rocket effect are calculated. The numerical scheme is tested by calculating the structure of both homogeneous bubbles and multiphase supernova remnants and comparing the results with already existing solutions.

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