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Dynamical evolution of a supernova driven turbulent interstellar medium

Published online by Cambridge University Press:  01 August 2006

Dieter Breitschwerdt  and
Miguel A. de Avillez
Dieter Breitschwerdt
Affiliation:
Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, A-1180 Vienna, Austria email: breitschwerdt@astro.univie.ac.at
Miguel A. de Avillez
Affiliation:
Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, A-1180 Vienna, Austria email: breitschwerdt@astro.univie.ac.at Department of Mathematics, University of Évora, R. Romão Ramalho 59, 7000 Évora, Portugal; email: mavillez@astro.univie.ac.at
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Abstract

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It is shown that a number of key observations of the Galactic ISM can be understood, if it is treated as a highly compressible and turbulent medium, energized predominantly by supernova explosions (and stellar winds). We have performed extensive numerical high resolution 3D hydrodynamical and magnetohydrodynamical simulations with adaptive mesh refinement over sufficiently long time scales to erase memory effects of the initial setup. Our results show, in good agreement with observations, that (i) volume filling factors of the hot medium are modest (typically below 20%), (ii) global pressure is far from uniform due to supersonic (and to some extent super-Alfvénic) turbulence, (iii) a significant fraction of the mass (~60%) in the warm neutral medium is in the thermally unstable regime (500 < T < 5000 K), (iv) the average number density of Ovi in absorption is 1.81 × 10−8 cm−3, in excellent agreement with Copernicus and FUSE data, and its distribution is rather clumpy, consistent with its measured dispersion with distance.

Keywords

ISM: generalISM: evolutionISM: structureISM: magnetic fieldshydrodynamicsMHDturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 57 - 64
Copyright
Copyright © International Astronomical Union 2007

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