| |
 |
| Paper: |
Modeling of Solar Active Region Using a Three-Dimensional, Time-Dependent, Data-Driven Magnetohydrodynamic Model |
| Volume: |
459, 6th International Conference of Numerical Modeling of Space Plasma Flows (ASTRONUM 2011) |
| Page: |
254 |
| Authors: |
Wu, S. T.; Wang, A. H.; Falconer, D.; Hu, Q.; Liu, Y.; Feng, X.; Shen, F. |
| Abstract: |
A self-consistent, three-dimensional magnetohydrodynamic model
together with time-dependent boundary conditions based on the
method of characteristics at the bottom boundary (photosphere) to
accommodate the observation will be discussed. To illustrate this
model, Active Region 11117 observed by SDO/HMI is chosen for the
analyses in that the magnetic field structures and evolution of
this active region will lead to the determination of the
conditions for the initiation of a solar eruption. Specific
physical parameters to be simulated are non-potential magnetic
field properties (i.e. emergence of magnetic flux (φ), the
length of magnetic shear of the main neutral line (Lss), and
the total current helicity (Hc) injected into the corona). We
have found that all the non-potential magnetic field properties
are necessary conditions for a solar eruptive event, but a
sufficient condition is revealed for AR11117 similar to the AR
10720 given by Wu et al. (2009). This sufficient condition is the
“fragmentation” of the magnetic shear along the neutral line. |
|
|
|
|
|
