| Original Articles |
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Envelope Soliton in Solar Radio Emission |
| WANG De-Yu1,2;G . P. Chernov3 |
| 1Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008
2National Astronamical Observatories, Chinese Academy of Sciences
3IZMIRAN, 142092 Troitask, Moscow Region, Russia
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| Cite this article: |
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WANG De-Yu, G . P. Chernov 2000 Chin. Phys. Lett. 17 355-357 |
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Abstract Several envelope soliton fine structures have been observed in solar radio metric-wave emission. We present a model of longitudinal modulational instability to explain these fine structures. It is found that this instability can only occur in the condition of sound velocity being larger than Alfvén velocity in corona. Therefore, the envelope soliton fine structures should display in the coronal region with high temperature and low magnetic field, which corresponds to the solar radio emission in the region of meter and decameter wavelength.
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| Keywords:
52.40.Db
52.35.Mw
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Published: 01 May 2000
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| PACS: |
52.40.Db
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(Electromagnetic (nonlaser) radiation interactions with plasma)
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52.35.Mw
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(Nonlinear phenomena: waves, wave propagation, and other interactions (including parametric effects, mode coupling, ponderomotive effects, etc.))
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