How do cosmic rays change their energy in the solar wind?The diffusion-convection (modulation) equation is derived directly from the Boltzmann equation on the basis of a minimum number of assumptions concerning the scattering process, among which are: (1) that the scattered particles undergo no energy change, and (2) that isotropy is an equilibrium state. It is noted that, in the event that the background plasma contains a magnetic field and the flow speeds of the plasma and scattering centers are different, additional terms arise that will modify the equations. If, moreover, the scatterers have individual motions relative to their average flow, the second-order Fermi acceleration term will appear.
Document ID
19850040703
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Jones, F. C. (NASA Goddard Space Flight Center Laboratory for High Energy Astrophysics, Greenbelt, MD, United States)