A brief review of the theoretical development of the planetary dynamo problem and theoretical models of the solar wind-magnetosphere interaction, such as the reconnection, viscous interaction and impulsive penetration models, is given. MHD mesoscale physics in the non-uniform plasma interaction region should be applied in order to understand how the energy of motion of the magnetofluids is transferred into electromagnetic (E-M) energy. A macro-particle description involving compressional and shear Alfvenons has been introduced to give the particle-like behavior of the corresponding MHD waves [Song and Lysak, 1994]. The driven nature of the solar windmagnetosphere interaction and driven reconnection are discussed in terms of the interactions between Alfvenons and between Alfvenons and the ambient magnetic field. A unified model of the solar wind-magnetosphere interaction may be established on the basis of Alfvenon dynamics.
|Original language||English (US)|
|Title of host publication||Physics of the Magnetopause, 1995|
|Editors||P. Song, M.F. Thomsen, B.U.O. Sonnerup|
|Publisher||Blackwell Publishing Ltd|
|Number of pages||8|
|State||Published - 1995|
|Name||Geophysical Monograph Series|
Bibliographical noteFunding Information:
Acknowledgments. We would like to thank B. U. O. Sonnerup for very helpful suggestions and comments on the paper. We have also benefited from discussions with many of our colleagues, including C. Cattell, W. Dai, R. Elphic, G. Fasel, K.-H. Glassmeier, J. T. Gosling, W. J. Heikkila, H. Kawano, H. Kuo, G. Le, J. Lemaire, N. Lin, T. Lui, R. N. Lundin, Z. Ma, P. Newell, A. Otto, E. N. Parker, T.-D. Phan, T. A. Potemra, G. Rostoker, C. T. Russell, D. Sibeck. This work has been sup ported in part by NSF Grants ATM-9111791 and ATM-9301043 and by NASA Grants NAGW-2653 and NAGW-2690.
© 1995 by the American Geophysical Union.