Solving the Equations of Magnetohydrodynamic in Three Dimensions to Study the Origin and Evolution of Turbulence in the Solar Wind
Abstract
In this tutorial we demonstrate an approach to modeling the origin and evolution of spatial and temporal fluctuations in the solar wind. One goal of this study 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 Alfv´enic fluctuations as opposed to quasi-two-dimensional fluctuations to determine the type of fluctuations that in the solar wind. We will discuss challenges associated with representing accurately the global heliospheric magnetic fields associated with the heliospheric current sheet (HCS) and how broadband fluctuations can be introduced as in-flow boundary conditions into a rotating heliosphere.
- Publication:
-
Space Plasma Simulation
- Pub Date:
- 2001
- Bibcode:
- 2001sps..proc..128G