Computer Science
Scientific paper
Jan 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.547..345o&link_type=abstract
Proceedings of 'SOHO 13 - Waves, Oscillations and Small-Scale Transient Events in the Solar Atmosphere: A Joint View from SOHO a
Computer Science
1
Scientific paper
Theoretical studies of the solar wind outflow in open magnetic structures motivated by SOHO observations indicate that both, high frequency ion-cyclotron waves and low frequency MHD waves play a role in the acceleration and heating of the solar wind plasma. In particular, the high temperature anisotropy of O5+ ions deduced from SOHO UVCS observations suggests that resonant heating due to ion cyclotron waves is important in minor ions. However, there are theoretical difficulties with the ion-cyclotron wave heating model of protons. It appears that low-frequency waves are still required to transport energy and to accelerate the solar wind on large scales. In addition, the source of electron heating is still an open question. I will review some of the recent wave heating models of the fast solar wind. I will discuss the threefluid model, that describes electrons, protons, and heavy ions as coupled fluids. This description allows to model different properties and heating processes for each particle species and to model the high temperature of the heavy ions in accordance with observations. I will show the results of 2.5D three-fluid, simulations of the solar wind plasma that combine the effects of MHD waves selfconsistently, and ion-cyclotron waves empirically as the sources of energy. I will review several results of hybrid kinetic models of ion-cyclotron wave heating and relaxation of heavy ion anisotropy.
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