Physics
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..109..149t&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 109, no. 1, 1987, p. 149-186.
Physics
68
Astronomical Models, Kolmogoroff Theory, Magnetohydrodynamic Waves, Particle Flux Density, Power Spectra, Solar Wind, Boundary Value Problems, Conductive Heat Transfer, Coronal Holes, Frequency Ranges, Helios Satellites, High Frequencies
Scientific paper
A model including the Alfvenic fluctuation power spectrum equation of Tu et al. (1984) is proposed which describes, under certain assumptions, the major properties of the radial evolution of the spectrum of the fluctuations observed by Helios in the 0.3-1 AU space range. Although solutions passing through the innermost critical point of the rapidly diverging flow geometry with f(max) = 7 have been found, there is too little pressure at the coronal base for comparison with the observational constraints. Results indicate that the cascade process can give considerable dissipation of the Alfvenic fluctuations. It is suggested that the momentum addition from the Alfvenic fluctuation pressure on the solar wind flow in the space range for r of less than 10 solar radii may provide significant acceleration, allowing the solutions to meet observational constraints at the coronal base and at 1 AU. The predicted energy cascade flux is found to be near the heating rate of the solar wind protons observed by Helios.
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