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A. Lazarian, H. Yan (U. Wisconsin)
Understanding of properties of MHD turbulence is essential for understanding of dynamics and acceleration of cosmic rays. We shaw that the scattering of cosmic rays happens at mostly by fast modes, while other componets of MHD turbulence are inefficient. We calculate rates of cosmic ray scattering as well as diffusion coefficeints for cosmic rays in different phases of ISM. We discuss how the presence of turbulence modifies streaming instability of cosmic rays and calculate the resulting spectrum.
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.