Aging of solar wind magnetic and velocity fluctuations from observations in the inner heliosphere

Details Aging of solar wind magnetic and velocity fluctuations from observations in the inner heliosphere Aging of solar wind magnetic and velocity fluctuations from observations in the inner heliosphere

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh41b1783r&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH41B-1783

Physics

[2149] Interplanetary Physics / Mhd Waves And Turbulence

Scientific paper

The heliosphere is a natural laboratory to study several aspects of Magnetohydrodynamic (MHD) turbulence. MHD fluctuations are ubiquitous in the solar wind (SW) and 'in situ' observations of plasma properties and magnetic field are one of the keys to unveil the secrets of MHD turbulence. In the interplanetary medium, MHD scale fluctuations are usually anisotropic, and these fluctuations frequently present different properties in regions of quasi-stationary SW with different bulk plasma parameters, or in regions associated with the presence of transients (e.g., magnetic clouds). It is known that the spatial structure of magnetic and velocity correlation functions evolves in the inner heliosphere. This evolution in terms of the aging of plasma parcels, as observed by the spacecrafts Helios 1-2, is the subject of the work presented here. Particular interest is put on the evolution of anisotropies in the integral length scale. Results are consistent with driving modes with wavevectors parallel to the direction of the local mean magnetic field near Sun, and a progressive spectral transfer of energy to modes with perpendicular wavevectors. Advances made in this direction, as those presented here, will be usefull to refine models used to describe the propagation and diffusion of charged solar and galactic energetic particles in the inner heliosphere, and will contribute to understand the MHD Alfvenic wave activity for this system.

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