MAGNETIC TURBULENCE IN THE HELIOSPHERE AND MAGNETIC CONNECTION FROM THE SUN TO THE EARTH

摘要

Magnetic fluctuations in the heliosphere are the result of photospheric motions, magnetic activity in the solar corona, and solar wind evolution and convection. Understanding the formation and evolution of magnetic turbulence, including features like the spectral index, the fluctuation level, the degree of anisotropy, as a function of heliographic distance, latitude, and stream structure, is a basic issue for magnetohydrodynamic turbulence studies. The Solar Orbiter can give a fundamental contribution to this field. In this paper we discuss the evolution of magnetic turbulence in the heliosphere, and show how knowledge of the above mentioned parameters allows to trace the magnetic field lines from the Sun to the Earth, a problem of interest to Space Weather predictions of solar energetic particle events.