Turbulencia MHD en la heliosfera interna

RUIZ M.E.; DASSO, S.; MATTHAEUS, W.H.; MARSCH, E.; WEYGAND, J. M.

San Juan

Conferencia; Reunión anual de la asociación argentina de astronomía; 2008

Asociación Argentina de Astronomía

The dynamical evolution of solar and galactic cosmic rays in the heliosphere issignificantly affected by the magnetic conditions of the medium. These effectsarise mainly from a combination of (i) the large-scale magnetic field configuration(which just acts as a guide for charged particles) and (ii) the small-scale fluctuations(which cause abrupt changes in their energy and/or momentum, known as wave-particle interaction). Magnetic fluctuations developed in the system in a spatial rangelarger than the ion skin depth can be modeled using the framework of MHD turbulence.In this work, we present a study of the turbulent properties in the inner heliosphere(solar wind between 0.3 and 1 astronomical unit) based on modeling {it in situ} plasmaand magnetic observations collected by Helios 1 and Helios 2 spacecraft throughout onefull eleven-year solar cycle. In particular we study the magnetic anisotropy properties in theinertial range.