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| Paper: |
Tsallis Statistics for Models and Observations of the Heliospheric Magnetic Field |
| Volume: |
406, Numerical Modeling of Space Plasma Flows: ASTRONUM - 2008 |
| Page: |
181 |
| Authors: |
Burlaga, L.F. |
| Abstract: |
The solar wind is a driven, open, non-linear, non-equilibrium, complex system. Streams, slow flows, ejecta, shocks, etc. produced near the Sun interact as they move away from the sun to create an evolving complex multiscale structure. During solar maximum, interaction regions merge with increasing distance from the sun, and these merged interaction regions coalesce form Global Merged Interaction Regions (GMIRs) which grow out to ≈ 45 AU and then decay out to ≈ 90 AU. One aspect of the statistical structure of the observed fluctuations of the magnetic strength B as a function of distance from the sun and scale can be described by the evolution of the probability distributions of increments of B, which can be described by the q-Gaussian functions of Tsallis statistics. These PDFs can be predicted by a deterministic 1-D multi-fluid MHD model with appropriate boundary conditions. |
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