The evolution and interaction of multiple coronal mass
Abstract
The famous solar events of Halloween 2003 caused two of the most intense geomagnetic storms with Dst min -363 and -401 nT during Solar Cycle 23 In order to understand the interplanetary causes of this famous event which contains multiple flares and coronal mass ejections we will perform MHD simulations to investigate the evolution of solar disturbances that caused these severe geomagnetic storms This study performs simulations of interplanetary coronal mass ejection ICME propagation in a realistic 3D solar wind structure from the Sun to the Earth by using the newly developed hybrid code HAFv 2 3DMHD This code combines two simulation codes Hakamada-Akasofu-Fry code HAF version 2 HAFv 2 and a fully three-dimensional time-dependent MHD simulation code and is used for this purpose The solar wind structure is simulated out to 0 08 AU 18 solar radius from source surface maps 2 5 solar radii Rs that are derived from daily-provided solar magnetograms using the HAFv 2 code This code is then used from 2 5 Rs to provide input for the lower boundary of the 3D MHD code to calculate the evolution of solar wind plasma and interplanetary magnetic field beyond 18 Rs 0 08 AU A dynamic disturbance mimicing a particular flare s energy output is delivered to this non-uniform structure to model the evolution and interplanetary propagation of coronal mass ejections ICME including their shocks We also integrate the line-of-sight density in the plane-of-sky to
- Publication:
-
36th COSPAR Scientific Assembly
- Pub Date:
- 2006
- Bibcode:
- 2006cosp...36..407W