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Magnetoacoustic Waves in the Solar Stratified Atmosphere
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| ZHENG Hui-Na1n;WANG Shui1;S. T. Wu2;LI Bo1 |
| 1Department of Earth and Space Sciences, University of Science and Technology of China, Hefei 230026
2Center for Space Plasma and Aeronomic Research and Department of Mechanical Engineering, University of Alabama in Huntsville, Huntsville, AL 35899, USA
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| Cite this article: |
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ZHENG Hui-Nan, WANG Shui, S. T. Wu et al 2001 Chin. Phys. Lett. 18 1624-1627 |
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Abstract 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.
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| Keywords:
52.30.Cv
96.60.-j
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Published: 01 December 2001
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| PACS: |
52.30.Cv
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(Magnetohydrodynamics (including electron magnetohydrodynamics))
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96.60.-j
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(Solar physics)
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