Physics
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh42c0549h&link_type=abstract
American Geophysical Union, Fall Meeting 2003, abstract #SH42C-0549
Physics
2159 Plasma Waves And Turbulence, 2164 Solar Wind Plasma, 7509 Corona
Scientific paper
Microwave radio scattering and scintillation observations reveal a variety of distinctive characteristics in the density fluctuation spectrum and scintillation velocity field of the solar wind inside 25 solar radii. Any plasma wave or turbulence model of the corona and solar wind must be consistent with these radio results as well as with in situ spacecraft measurements outside 60 solar radii. High-frequency Alfven (ion-cyclotron) waves have some distinctive properties whose signatures appear to be showing up in the radio data. Obliquely propagating Alfven waves have substantial compressibility at high frequency that can explain the observed flattening of the density spectrum at 10-100 km scales, provided that there is an additional power-law component of passive density fluctuations riding on the magnetic turbulence. Proton cyclotron and electron Landau damping of the waves can account for the inner scale in the density spectrum as well as the observed break in spacecraft magnetic spectra, although an active Kolmogorov cascade is required to counteract spectrum erosion from wave damping. Such a cascade implies an energy input from wave dissipation that is substantial and much greater than that associated with cyclotron sweep of a passive spectrum. Interplanetary scintillation velocity measurements show a large parallel random component and small perpendicular random component, which is consistent with Alfven waves and inconsistent with fast-mode waves. The parallel velocity spread could result from a combination of wave dispersion and line-of-sight variations in the Alfven speed. All of the above effects will be discussed on the basis of numerical modeling results obtained assuming an evolving angular spectrum of Alfven waves described by a kinetic Vlasov dispersion code.
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