Turbulent heating and temperature evolution in the solar wind plasma

摘要: We calculate the turbulent dissipation rate of incompressive hydromagnetic fluctuations and resulting radial evolution temperature in solar wind using generalizations Kolmogorov Kraichnan MHD turbulence phenomenologies that include suppression by high cross helicity. The results for are compared to a variety data sets test over wide parameter range. Motivated observations, we use different power laws radius amplitudes Alfvenic nonAlfvenic determine cascade rates. To explain observations Kolmogorov-like models, found it necessary suppress rates helicity streams even further than predicted simple models ; this may be due nonequilibrium nature spectrum or other causes as yet unknown. model gives rise significant amount heating, implying while likely dominant only inner heliosphere, competitive with heating shocks assimilation interstellar pickup ions outer heliosphere. In contrast, generalized phenomenology yields less seems inadequate observations. conclude no existing adequately explains observed dependence wind, there appears sufficient energy available contribute significantly,