Boundary Flows in Solar Active Regions

Details Boundary Flows in Solar Active Regions Boundary Flows in Solar Active Regions

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh51c..10g&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH51C-10

Physics

7513 Coronal Mass Ejections, 7519 Flares, 7524 Magnetic Fields, 7529 Photosphere

Scientific paper

We present a general technique to calculate the flow field at the altitude where vector magnetic field measurements of solar active regions have been obtained. The velocity field vector is reconstructed fully by solving the ideal induction equation of magnetohydrodynamics for the cross-field velocity component and by utilizing the Doppler velocity information to calculate the field-aligned velocity component. Because solving the induction equation is an under-determined problem, we have formulated our technique in such a way as to provide a unique solution of the induction equation when the vertical (normal to the boundary) component of the cross-field velocity is prescribed. We provide examples of various possible choices for the cross-field vertical velocity and we discuss the respective results. Moreover, we showcase the validity of our technique by predicting the particular area of NOAA active region 8210 from which a flare and a CME were triggered, using the reconstructed velocity field vector.

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