| Abstract : | Solar coronal transients, particularly the solar flares and coronal mass ejections, are the primary drivers of space weather. Generally, the transients are believed to be caused by magnetic reconnection: a process in which, magnetic field lines change their connectivity along with acceleration of charged particles and generation of heat. In absence of a reliable measurement, a novel procedure is to extrapolate the coronal magnetic field using photospheric magnetograms and subsequently use the same as an initial condition to explore magnetic field line dynamics and magnetic reconnection through numerical simulations. In the presentation, focus will be made on these data-constrained simulations, results and their limitations. |
