MHD Simulations of a Supernova-driven ISM and the Warm Ionized Medium

Type Conference Paper
Names Alex S. Hill, M. R. Joung, R. A. Benjamin, L. M. Haffner, C. Klingenberg, M. M. Mac Low, K. Waagan, K. A. Wood
Proceedings Title Bulletin of the American Astronomical Society
Conference Name American Astronomical Society, AAS Meeting #217, #251.06
Volume 43
Date January 1, 2011
Library Catalog NASA ADS
Abstract We present new 3D MHD simulations of a supernova-driven, stratified interstellar medium. We have previously shown that the density distribution arising from hydrodynamical versions of these simulations creates low-density pathways through which Lyman continuum photons can travel to heights |z| > 1 kpc. This naturally produces the warm ionized medium through photoionization due primarily to O stars near the plane. However, the hydrodynamical models reproduce the peak but not the width of the emission measure distribution observed in Wisconsin H-Alpha Mapper (WHAM) data. Here, we discuss the role of magnetic fields in the structure of gas away from the plane. We compare emission measure distributions from models with varying magnetic field strengths to the WHAM observations. The simulations were performed using the adaptive mesh refinement grid code FLASH with the new MHD solver developed by Waagan et al. This work was partly supported by NASA/SAO grant TM0-11008X and by NSF grant AST-0607512.
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