Statistics – Computation
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh51b..02h&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH51B-02
Statistics
Computation
2101 Coronal Mass Ejections (7513), 7513 Coronal Mass Ejections (2101), 7524 Magnetic Fields, 7900 Space Weather
Scientific paper
A boundary-layer model to treat the time-varying radial (normal) components of the solar surface magnetic field in the time-dependent three-dimensional MHD simulation of the global solar corona is proposed. In order to avoid the computational difficulties in calculating the vector quantities of the magnetic field and plasma motion on the computational boundary surface, we assumed the shallow spherical volume layer at the lowermost corona in which the "differential potential field" is added to the existing magnetic field so that the boundary magnetic field will be identical to the measured ones and the variation can satisfy the solenoidal condition. The differential potential field uses the differential synoptic map that is calculated by subtracting a synoptic map from the map of previous Carrington rotation. The assumed differential potential field can be regarded as representing the large-scale variation of the surface magnetic field. By gradually adding the differential potential field to the existing numerical coronal magnetic field, we can simulate the continuous coronal variations in the global scale and examine the responses of the coronal magnetic field and plasma to the global change of the boundary solar surface magnetic field. The coronal responses obtained with our model of the time-varying solar corona include (a) formations of twisted magnetic loops along the polarity inversion line, (b) formations of the condensed density regions at lower corona, mostly but not always at the twisted magnetic loop regions, (c) sudden changes of magnetic topology such as eruption of magnetic loops and coronal plasma.
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