Photospheric Dynamic Model of Magnetic Reconnection
Abstract
We present a dynamic model of the atmospheric magnetic field in which magnetic loop footpoints are controlled by photospheric flows computed through a N-body algorithm. This simulation reproduces a system whose behaviour is characterized by small scale (e.g., granular) advection flows that interact to form large spatial organization scales (e.g., meso- and super-granulation). In this model the passive advection of magnetic footpoints through photospheric spatio-temporal correlated flows causes the magnetic field to reconfigure as a consequence of magnetic reconnection processes. This approach, based on the dynamic model of multiple magnetic loops tep{b8 Hu03} and on an advective-interaction model proposed by tet{b8 Ra03}, naturally accounts for the observed probability distribution functions and waiting time statistics of the emitted magnetic energy.
- Publication:
-
Solar Polarization 4
- Pub Date:
- December 2006
- Bibcode:
- 2006ASPC..358...76B