Astronomy and Astrophysics – Astronomy
Scientific paper
May 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...194.6408m&link_type=abstract
American Astronomical Society, 194th AAS Meeting, #64.08; Bulletin of the American Astronomical Society, Vol. 31, p.925
Astronomy and Astrophysics
Astronomy
Scientific paper
Energy input from supernovae (SNe) and stellar winds maintains the hot component of the ISM, as well as maintaining the velocity dispersion in the warm medium at trans-Alfvenic velocities. The random nature of this input suggests that it generates ``turbulence''. Although chaotic motions are indeed generated, this supersonic, trans-Alfvenic turbulence cannot be described using the properties of incompressible hydrodynamic turbulence. Energy decays at a different rate, density contrasts appear, and self-similarity is not guaranteed. Direct numerical simulations of SN-driven turbulence have progressed, moving from the 2D simulations of the last decade to full 3D simulations with discrete blast wave driving in recent years. I will briefly review the highlights of these simulations, emphasizing that single structures are very difficult to interpret if the chaotic background medium is not taken into account. Simple clump models of turbulence that neglect the correlation of density and velocity structure are probably inadequate. I will show preliminary results of models of SN explosions in a uniformly driven turbulent medium to begin to address these issues.
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