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| Titel |
Hybrid models of solar wind plasma heating |
| VerfasserIn |
L. Ofman, A.-F. Viñas, P. S. Moya |
| Medientyp |
Artikel
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| Sprache |
Englisch
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| ISSN |
0992-7689
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| Digitales Dokument |
URL |
| Erschienen |
In: Annales Geophysicae ; 29, no. 6 ; Nr. 29, no. 6 (2011-06-20), S.1071-1079 |
| Datensatznummer |
250017041
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| Publikation (Nr.) |
 copernicus.org/angeo-29-1071-2011.pdf |
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| Zusammenfassung |
| Remote sensing and in-situ observations show that solar wind ions are often
hotter than electrons, and the heavy ions flow faster than the protons by up
to an Alfvén speed. Turbulent spectrum of Alfvénic fluctuations and
shocks were detected in solar wind plasma. Cross-field inhomogeneities in the
corona were observed to extend to several tens of solar radii from the Sun.
The acceleration and heating of solar wind plasma is studied via 1-D and 2-D
hybrid simulations. The models describe the kinetics of protons and heavy
ions, and electrons are treated as neutralizing fluid.The expansion of the
solar wind is considered in 1-D hybrid model. A spectrum of Alfvénic
fluctuations is injected at the computational boundary, produced by
differential streaming instability, or initial ion temperature anisotropy,
and the parametric dependence of the perpendicular heating of
H+-He++ solar wind plasma is studied. It is found that He++
ions are heated efficiently by the Alfvénic wave spectrum below the
proton gyroperiod. |
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