Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21533204b&link_type=abstract
American Astronomical Society, AAS Meeting #215, #332.04; Bulletin of the American Astronomical Society, Vol. 42, p.430
Astronomy and Astrophysics
Astrophysics
Scientific paper
MHD turbulence plays a key role in a variety of astrophysical phenomena, such as dynamics of ISM, stellar winds, propagation and acceleration of Cosmic Rays. We look into the most basic unresolved issues with MHD turbulence, namely the nature of Alfvenic cascade and imbalanced turbulence. We also study so-called small scale dynamo which is a process which quickly generates magnetic energy in a transient high-energetic events, such as supernova shocks. We discuss the general case of MHD turbulence, an imbalanced turbulence which eluded consistent description for a long time. We were able to pinpoint the mechanism by which the dominant wave's frequency increases along the cascade, the mechanism that is different from Goldreich-Sridhar critical balance. We successfully tested our model with high-resolution (up to 20483) direct numerical simulations of MHD turbulence in different regimes. We briefly discuss implications of our findings to the realistic compressible turbulence in the ISM and the Solar wind. We applied our findings in small-scale dynamo to the problem of diffusive shock acceleration (DSA) in the context of the strong shock precursor and strong perturbations of density in the inflowing fluid. It turns out that the magnetic fields generated by turbulent mechanism (i.e. small-scale dynamo) is significant and could be larger than magnetic fields generated by instability mechanisms such as Bell's instability. We calculated the properties of Cosmic Ray scattering and acceleration in such fields. I acknowledge support by ICECUBE project and the Center for Magnetic Self Organization (CMSO).
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