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Control of star formation by supersonic turbulence
Understanding the formation of stars in galaxies is central to much of modern astrophysics. However, a quantitative prediction of the star formation rate and the initial distribution of stellar
Starburst-driven Mass Loss from Dwarf Galaxies: Efficiency and Metal Ejection
We model the effects of repeated supernova (SN) explosions from starbursts in dwarf galaxies on the interstellar medium of these galaxies, taking into account the gravitational potential of their
The Energy Dissipation Rate of Supersonic, Magnetohydrodynamic Turbulence in Molecular Clouds
Molecular clouds have broad line widths, which suggests turbulent supersonic motions in the clouds. These motions are usually invoked to explain why molecular clouds take much longer than a free-fall
Superbubbles in disk galaxies
Correlated supernovae from an OB association create a superbubble: a large, thin, shell of cold gas surrounding a hot pressurized interior. Because supernova blast waves usually become subsonic
Comparing the statistics of interstellar turbulence in simulations and observations - Solenoidal versus compressive turbulence forcing
Context. Molecular clouds (MCs) exhibit supersonic turbulent velocity and density fluctuations on virtually all scales observed by modern telescopes. The origin and structural characteristics of this
Kinetic Energy Decay Rates of Supersonic and Super-Alfvénic Turbulence in Star-Forming Clouds
We compute 3D models of supersonic, sub-Alfvenic, and super-Alfvenic decaying turbulence, with an isothermal equation of state appropriate for star-forming interstellar clouds of molecular gas. We
WHAT IS DRIVING THE H I VELOCITY DISPERSION
Original article can be found at: http://www.iop.org/EJ/journal/1538-3881 Copyright American Astronomical Society. DOI: 10.1088/0004-6256/137/5/4424 [Full text of this article is not available in the
Superbubble blowout dynamics
Multiple supernovae and stellar winds from OB associations carve large holes filled with hot gas in the galactic disk. These superbubbles sweep up H I into cold, thin, dense shells and eventually
Shock interactions with magnetized interstellar clouds. 1: Steady shocks hitting nonradiative clouds
We study the interaction of a steady, planar shock with a nonradiative, spherical, interstellar cloud threaded by a uniform magnetic field. For strong shocks, the sonic Mach number scales out, so two
The Distribution of Pressures in a Supernova-Driven Interstellar Medium
Observations have suggested substantial departures from pressure equilibrium in the interstellar medium (ISM) in the plane of the Galaxy, even on scales under 50 pc. Nevertheless, multi-phase models
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