Other
Scientific paper
Sep 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..277g&link_type=abstract
SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 277-2
Other
1
Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Interplanetary Magnetic Fields
Scientific paper
The time-dependent response of the corona in a spherical shell between 1.8 and 16 Rs to injection of low-frequency Alfvén waves at the inner boundary is considered in the MHD, isothermal and axisymmetric framework, without approximation for the wave-wind coupling. The magnetic field is the sum of an external dipole field assumed to be produced by the sun and of the field induced by the plasma motion in the spherical shell. Due to Alfvén wave injection, the wind and magnetic structure change, leading to an increased overexpansion of the high-latitudes flows and fields. Some of the factors which affect these changes: dissipation, and latitudinal distribution of the waves are explored, and the quantitative relation between wind speed and wave amplitude are discussed. We conclude that Alfvén waves alone lead ultimately to the disappearance of the slow wind, and that other factors, such as transverse structures and compressive waves, are necessary to explain the observed structure of the solar wind.
Grappin Roland
Leorat Jacques
Rifai Habbal Shadia
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