ACE/Wind multispacecraft analysis of the magnetic correlation in the solar wind
The propagation of galactic and solar cosmic rays in the solar wind (SW) can be strongly influenced by the SW fluctuations properties. Magnetohydrodynamic scale fluctuations in the solar wind are usually highly anisotropic, and have also been found to exhibit different properties in regions of high...
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| Autores principales: | , , , , , , |
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| Formato: | CONF |
| Materias: | |
| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_NIS22749_v1_nSH_p625_Dasso |
| Aporte de: |
| Sumario: | The propagation of galactic and solar cosmic rays in the solar wind (SW) can be strongly influenced by the SW fluctuations properties. Magnetohydrodynamic scale fluctuations in the solar wind are usually highly anisotropic, and have also been found to exhibit different properties in regions of high and low solar wind speed. Previous studies analyzed the anisotropy properties of the solar wind magnetic fluctuations at scales of the order of (105 ? 106) km (inertial range) using two times ? single point measurements (assuming the Taylor frozen-in hypothesis), and found that the fluctuations in the fast solar wind tend to reside in wave vectors with their parallel component (to the mean magnetic field) larger than the perpendicular one, while the fluctuations in the slow wind present the opossite trend. In the present study we compare the magnetic autocorrelation function in the solar wind obtained with two times ? single point observations (from a single spacecraft) with the same quantity obtained from single time ? two points measurements (from simultaneous observations of two spacecraft, observing the pure spatial structures). We preliminarily compare also previous results of the anisotropy of the solar wind fluctuations, obtained from a single spacecraft, with our new multispacecraft analysis using combining observations from the ACE and Wind spacecraft. |
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