Other
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh41a..15s&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH41A-15
Other
2114 Energetic Particles (7514), 2159 Plasma Waves And Turbulence
Scientific paper
In a wide range of heliosphere physics problems the hydromagnetic turbulence produces an essential effect, which should be not only involved into a consideration, but also quantified. The latter is especially important for large multi-factorial numerical models of the Solar corona and inner heliosphere, pretending to describe and even to predict the state of the bi-modal solar wind, solar flares, coronal mass ejections, the interplanetary shock propagation. For the listed phenomena, the turbulent waves dissipation (a "turbulent heating") is believed to result in the solar wind powerization. The latter effect controls the whole magnetic configuration and the plasma flow pattern troughout the Solar system. In the inner Solar corona the momentum transfer from turbulent waves to the bulk plasma motion via thewave pressure is also important. Another realm of problems of heliospheric physics, in which the interaction with a weak hydromagnetic turbulence arises in a natural way, is the solar energetic particles acceleration by interplanerary shock waves. As long as the particles are believed to be accelerated by the first order Fermi acceleration, the essential effect is the particle scattering by the hydromagnetic turbulence. This is because the essence of the first order Fermi acceleration is that the particle, randomly scattered by the turbulent magnetic field, can appear to be capturted for some time in the vicinity of the shock wave front, gaining the kinetic energy at each scattering from downstream of the shock front to upstream and back. To quantify this process one needs to find the level of turbulence excited by the suprathermal protons in the vicinity of the shock wave front, what requires to involve the equation for the turbulent waves transport. Here we derive the transport equation for turbulent waves, in particular for hydromagnetic Alfvénic turbulence. We demonstrate the way to integrate this model into a global framework suited for space weather simulations. This may be used both in numerical studies of the solar wind acceleration and heating as well as in models for production and transport of SEPs (solar energetic particles).
Roussev Ilia I.
Sokolov Iu. I.
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