Magnetic Reconnection Induced by Convective Intensification of Solar Photospheric Magnetic Fields

Abstract

We investigate photospheric magnetic reconnection induced by convective intensificd ..ation of solar surface magnetic fields, performing 2.5-dimensional magnetohydrodynamic (MHD) numerical simulations. We assume as the initial conditions oppositely directed vertical weak magnetic fields (Bz) penetrating a convectively unstable layer. To initiate convective instability, the unstable layer is perturbed by weak circular motions. As a result of the growing convective motions, the oppositely directed magnetic fields are swept up into the convective downflow region, forming a current sheet between them. At the same time, the field strength is increased to kilogauss range, and the current density in the current sheet is strengthened. As a result, magnetic reconnection is initiated.