Suzie
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Why the temperatures in the solar wind are almost the same in certain directions, and why different energy densities are practically identical, was until now not clear. With a new approach to calculating instability criteria for plasmas, Bochum researchers led by Prof. Dr. Reinhard Schlickeiser (Chair for Theoretical Physics IV) have solved both problems at once. They were the first to incorporate the effects of collisions of the solar wind particles in their model. This explains experimental data significantly better than previous calculations and can also be transferred to cosmic plasmas outside our solar system.
The plasma beta represents the ratio of kinetic to magnetic pressure in the cosmic plasma. The anisotropy is the ratio of the perpendicular and parallel temperatures to the magnetic field lines. The number of measured values is shown in colour (red corresponds to many values, blue to few values). Why the measurements take on the characteristic rhombic shape is explained by a new model by Bochum
The plasma beta represents the ratio of kinetic to magnetic pressure in the cosmic plasma. The anisotropy is the ratio of the perpendicular and parallel temperatures to the magnetic field lines. The number of measured values is shown in colour (red corresponds to many values, blue to few values). Why the measurements take on the characteristic rhombic shape is explained by a new model by Bochum