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• W2085594232 abstract "During the onset of coronal mass ejections, a front of enhanced EUV emission is sometimes seen to propagate away from a flaring active region across the solar disk. We present model simulations to test the hypothesis that these transients (called EIT waves) represent fast-mode MHD waves. The distribution of the magnetosonic velocity vf in the corona is determined using a current-free extrapolation of the measured photospheric field and a density scaling law for coronal loops. In agreement with observations, the waves are deflected away from active regions and coronal holes, where vf is large; they are also refracted upward as they propagate away from their initiation point, since vf falls off rapidly above active regions. The average surface-projected expansion speeds are only of order 200 km s-1, comparable to or somewhat smaller than those of EIT waves observed during 1997-1998. The model is unable to account for the velocities in excess of 600 km s-1 associated with Moreton waves and type II radio bursts unless it is assumed that the initial disturbance has the form of a strong, super-Alfvénic shock." @default.
• W2085594232 created "2016-06-24" @default.
• W2085594232 creator A5084940816 @default.
• W2085594232 date "2000-11-01" @default.
• W2085594232 modified "2023-09-25" @default.
• W2085594232 title "EIT Waves and Fast-Mode Propagation in the Solar Corona" @default.
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• W2085594232 doi "https://doi.org/10.1086/318178" @default.
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