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Paper: Coronal Heating and Acceleration of the Fast/Slow Solar Wind by Fast/Slow MHD Waves
Volume: 325, The Solar-B Mission and the Forefront of Solar Physics
Page: 263
Authors: Suzuki, T.K.
Abstract: We investigate coronal heating and acceleration of the high- and low-speed solar wind in the open field region by dissipation of fast and slow magnetohydrodynamical (MHD) waves through MHD shocks. Linearly polarized Alfvén (fast MHD) waves and acoustic (slow MHD) waves traveling upwardly along with a magnetic field line eventually form fast switch-on shock trains and hydrodynamical shock trains (N-waves) respectively to heat and accelerate the plasma. The heating from the slow waves is effective in the low corona to increase the density there, and plays an important role in the formation of the dense low-speed wind. On the other hand, the fast waves can carry a sizable energy to the upper level to heat the outer corona and accelerate the high-speed wind effectively. Accordingly, the rms shock amplitude of the transverse mode is larger in the high-speed wind, while that of the longitudinal mode is larger in the low-speed wind.
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