Physics
Scientific paper
Jan 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...40..193h&link_type=abstract
Solar Physics, vol. 40, Jan. 1975, p. 193-216.
Physics
11
Astronomical Models, Electron Distribution, Plasma Waves, Solar Corona, Type 3 Bursts, Wave Excitation, Atmospheric Models, Diffusion Coefficient, Magnetohydrodynamic Stability, Solar Atmosphere, Solar Physics, Velocity Distribution
Scientific paper
An exciter model is proposed which would be consistent with the fact that the energetic particles ejected from the sun and which initiate the process leading to radio burst emission are often observed to travel to large distances from the sun. If one assumes the plasma wave hypothesis of radio burst emission, plasma wave instability, however, should rapidly stop the particle beam. The present model shows that stabilization of the exciter electron distribution is facilitated when the coronal electron density decreases with altitude faster than the inverse of the square of the altitude. The stabilized part of the exciter electron distribution is gradually eroded away as the exciter propagates through the coronal plasma. This erosion provides the energy to excite the plasma waves associated with the type-III radioburst. Using a simple model for the distribution of electrons ejected from the sun, the maximum of the spatial density of the power converted into plasma waves is found to move at a constant speed determined by the velocity distribution of the ejected electrons.
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