Alfvén Wave Reflection and Turbulence in the Solar Corona and Solar Wind

Details Alfvén Wave Reflection and Turbulence in the Solar Corona and Solar Wind Alfvén Wave Reflection and Turbulence in the Solar Corona and Solar Wind

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh21b0157v&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH21B-0157

Mathematics

Logic

7509 Corona, 7863 Turbulence

Scientific paper

We solve the equations for Alfvén wave propagation along the magnetic field from the base of the solar corona into the solar wind using a phenomenological term for nonlinear interactions and dissipation, along the lines of Dmitruk et al. 2002. Wave reflection due to the gradients in the Alfvén and solar wind speed is explicitly taken into account as a source for the nonlinear interactions, and regularity boundary conditions at the Alfvénic critical point are imposed. Within the corona, most of the wave reflection and nonlinear interactions occur close to the solar base, though the dependence on outward wave amplitude is non-trivial. Models in which interacting waves have comparable frequencies are considered as well as models in which the interaction depends on the full spectrum of inward and outward propagating modes. The relevance of Alfvén wave reflection as a source for turbulent heating of coronal holes and the fast solar wind is discussed, and our results are compared to previous work on the same topic. Dmitruk,ÿP.; Matthaeus,ÿW.ÿH.; Milano,ÿL.ÿJ.; Oughton,ÿS.; Zank,ÿG.ÿP.; Mullan,ÿD.ÿJ., 2002, ``Coronal Heating Distribution Due to Low-Frequency, Wave-driven Turbulence", ApJ 575, 571.

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