摘要
The propagation of magnetoacoustic waves in the solar atmosphere consisting of the photosphere, chromosphere and corona has been studied numerically by time-dependent multi-dimensional magnetohydrodynamic (MHD) simulation. Pressure disturbances are introduced at the bottom of the chromosphere and at the bottom of the corona, respectively. The computational results show that incurred fast and slow MHD waves propagate away from the source of the disturbances. The fast MHD wave propagates as an expansive wave in the radial direction, while the slow one steepens and it may evolve into a slow shock. We suggest that the extreme ultraviolet imaging telescope wave observed by the SOHO and Moreton wave are a fast MHD wave propagating in the corona and in the chromosphere, respectively.
作者
ZHENG Hui-Nan
WANG Shui
S.T.Wu
LI Bo
郑惠南;王水;吴式灿;李波(Department of Earth and Space Sciences,University of Science and Technology of China,Hefei 230026;Center for Space Plasma and Aeronomic Research and Department of Mechanical Engineering,University of Alabama in Huntsville,Huntsville,AL 35899,USA)
基金
Supported by the National Natural Science Foundation of China under Grant No.49834030
the Department of Science and Technology of China(G2000078405).
