Abstract
The EBM equations assume the MHD closure, that is, that proton temperature is isotropic. This assumption is not always valid. As it can be seen from 2D cuts of the 3D velocity distribution functions of protons, while the core of the velocity distribution function for slow winds is isotropic, the distribution for fast winds is perpendicular to the mean magnetic field axis. Consequently, temperature anisotropy is more important for fast winds than for slow winds. Here, we propose how to take into account this property of the solar wind that has not been considered in this thesis.
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Montagud-Camps, V. (2019). Future Work: Temperature Anisotropy Description . In: Turbulent Heating and Anisotropy in the Solar Wind. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-030-30383-9_14
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DOI: https://doi.org/10.1007/978-3-030-30383-9_14
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