Supernova-Driven Interstellar Medium Simulations: Velocity Dispersion and Density Structure

Details Supernova-Driven Interstellar Medium Simulations: Velocity Dispersion and Density Structure Supernova-Driven Interstellar Medium Simulations: Velocity Dispersion and Density Structure

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.6104j&link_type=abstract

American Astronomical Society Meeting 204, #61.04; Bulletin of the American Astronomical Society, Vol. 36, p.769

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Hydrodynamic feedback from massive stars in the form of supernovae appears to play a crucial yet poorly understood role in many processes, including star formation inside molecular clouds, the formation of galactic-scale outflows, and chemical enrichment of the ISM and the IGM. We present first results from three-dimensional simulations of the ISM structured by realistic driving due to isolated and correlated supernovae in the disk. We use FLASH, an Eulerian piecewise-parabolic method hydrodynamics code with adaptive mesh refinement capability. Interactions between multiple supernova remnants in the plane form substantial regions of high pressure and density even in the absence of self-gravity. We compare the vertical density distribution to observed values. We further measure the effective velocity dispersion and turbulent pressure as a function of given supernova rate. This yields a parameter vital for cosmological simulations that need to include the effects of feedback from star formation.
MKRJ was supported by an AMNH Graduate Student Fellowship. M-MML was partially supported by NSF grants AST 99-85392 and AST 03-07854. The software used in this work was in part developed by the DOE-supported ASCI/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago. Computations were performed at the Pittsburgh Supercomputing Center.

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