Numerical simulations of Galactic dynamo in a turbulent and shearing interstellar medium.
Princeton has a long tradition of excellence in the field of plasma astrophysics, dating back to Lyman Spitzer's pioneering work on the physical properties of interstellar gas. Rapid accretion rates are commonly observed in many kinds of accretion disks and are necessarily accompanied by rapid transport of angular momentum.
Often turbulence is evoked for this purpose. The detailed mechanisms to generate the needed turbulence is an active topic of investigation at Princeton. Detailed mechanisms for forming a shock and converting flow energy into particle thermal energy are of interest in order to interpret the observed emissions from supernova explosions and their remnants.
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These shocks are often collisionless, in the sense that the collisional mean free path is much larger than shock thickness. For example, particle acceleration is determined by turbulence spectra that in turn depends on the energy distribution of the accelerated particles.
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The authors also give theoretical results based on many calculations analysis of observational data: Tsytovich contributes new theoretical calculations. This book can prove helpful for nuclear scientists and researchers working with plasma physics or astro-physics. We are always looking for ways to improve customer experience on Elsevier. We would like to ask you for a moment of your time to fill in a short questionnaire, at the end of your visit. If you decide to participate, a new browser tab will open so you can complete the survey after you have completed your visit to this website.
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