Simulations of MHD turbulence in the solar wind: challenges and comparisons with observations
Abstract
Constructing realistic simulations of the magnetohydrodynamic (MHD) turbulence in the solar wind requires at least two elements. First, it is essential to model the three-dimensional structure of the heliosphere, including fast and slow flows, a tilted, rotating current sheet, and a global magnetic field that is an appropriate solution of the MHD equations. The second element is to formulate the in-flow of waves and or static structures into this volume. In this talk we review briefly our approach to this task. One of our goals is to determine how temporal and spatial fluctuations incident into the solar wind from the solar corona evolve in the heliosphere. In addition, we use the simulations to elucidate the distinguishing properties of Alfvénic fluctuations and quasi-two-dimensional fluctuations to determine the type of fluctuations that exist in the solar wind. We will discuss challenges associated with representing accurately the global heliospheric magnetic fields associated with the heliospheric current sheet and how broadband fluctuations, introduced as in-flow boundary conditions into a rotating heliosphere, evolve in the presence of velocity shear. The simulations will be compared with in situ observations of the magnetic field and plasma.
- Publication:
-
APS Division of Plasma Physics Meeting Abstracts
- Pub Date:
- October 2001
- Bibcode:
- 2001APS..DPPKM1003G