- Conference date: 15-18 April 1996
- Location: Marlboro, Massachusetts (USA)
The mechanisms responsible for the solar corona and the high-speed solar wind streams are still not known. Traditional wave-driven solar wind models do not seem capable of producing the rapid acceleration of the wind close to the Sun, which is implied by recent remote sensing data. A variety of new ideas have been put forth. In one class of models, the coronal protons (and perhaps also the heavier ions, such as helium nuclei) are preferentially heated to temperatures substantially in excess of the electrons; high-frequency ion-cyclotron waves, MHD shocks, and/or MHD turbulence may induce the ion heating. Another class of models invokes transitory field-aligned jets at the coronal base. In both of these types of models, magnetic reconnection events may be the fundamental energy source. In another class of models, electric fields and gravity act as velocity filters which allow only high-speed particles to reach the corona and solar wind. The Solar Probe should be able to detect remnants and signatures of the processes which heat the corona and accelerate the solar wind.
- Solar corona
- Solar wind
- Turbulence simulations
- Alpha particles
Y. K. Semertzidis, M. Aoki, M. Auzinsh, V. Balakin, A. Bazhan, G. W. Bennett, R. M. Carey, P. Cushman, P. T. Debevec, A. Dudnikov, F. J. M. Farley, D. W. Hertzog, M. Iwasaki, K. Jungmann, D. Kawall, B. Khazin, I. B. Khriplovich, B. Kirk, Y. Kuno, D. M. Lazarus, L. B. Leipuner, V. Logashenko, K. R. Lynch, W. J. Marciano, R. McNabb, W. Meng, J. P. Miller, W. M. Morse, C. J. G. Onderwater, Y. F. Orlov, C. S. Ozben, R. Prigl, S. Rescia, B. L. Roberts, N. Shafer‐Ray, A. Silenko, E. J. Stephenson, K. Yoshimura and EDM Collaboration
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