MHD Modeling of Coronal Hole Evolution
Abstract
MHD simulations of the solar corona based on maps of the solar magnetic field have been demonstrated to describe many aspects of coronal structure. However, these models are typically integrated to steady state, using synoptic or daily-updated magnetic maps to derive the boundary conditions. The Sun's magnetic flux is always evolving, and these changes in the flux affect the structure and dynamics of the corona and heliosphere. In this presentation, we describe an approach to evolutionary models of the corona and solar wind, using time-dependent boundary conditions. A key aspect of our approach is the use of the Air Force Data Assimilative Photospheric flux Transport (ADAPT) model to develop time-evolving boundary conditions for the magnetic field. In this study, we use a simplified (zero-beta) MHD model to investigate coronal hole evolution during the June-August 2010 time period (Carrington rotations 2098-2099). We compare modeled and observed coronal holes, and discuss implications of coronal hole evolution for the origin of the slow solar wind.
- Publication:
-
American Astronomical Society Meeting Abstracts #224
- Pub Date:
- June 2014
- Bibcode:
- 2014AAS...22432336L