Nonlinear Processes in Geophysics www.nonlin-processes-geophys.net 1023-5809 1607-7946 12 2 2005 10.5194/npg-12-299-2005 http://www.nonlin-processes-geophys.net/12/299/2005/ http://www.nonlin-processes-geophys.net/12/299/2005/npg-12-299-2005.html http://www.nonlin-processes-geophys.net/12/299/2005/npg-12-299-2005.pdf 299 310 2005-02-17 Parallel and perpendicular cascades in solar wind turbulence S. Oughton W. H. Matthaeus Department of Mathematics, University of Waikato, Hamilton, New Zealand Bartol Research Institute, University of Delaware, Newark, DE 19716, USA MHD-scale fluctuations in the velocity, magnetic, and density fields of the solar wind are routinely observed. The evolution of these fluctuations, as they are transported radially outwards by the solar wind, is believed to involve both wave and turbulence processes. The presence of an average magnetic field has important implications for the anisotropy of the fluctuations and the nature of the turbulent wavenumber cascades in the directions parallel and perpendicular to this field. In particular, if the ratio of the rms magnetic fluctuation strength to the mean field is small, then the <I>parallel wavenumber cascade is expected to be weak</I> and there are difficulties in obtaining a cascade in frequency. The latter has been invoked in order to explain the heating of solar wind fluctuations (above adiabatic levels) via energy transfer to scales where ion-cyclotron damping can occur.Following a brief review of classical hydrodynamic and magnetohydrodynamic (MHD) cascade theories, we discuss the distinct nature of parallel and perpendicular cascades and their roles in the evolution of solar wind fluctuations.