  We propose a reconnection-condensation model in which topological change in a
coronal magnetic field via reconnection triggers radiative condensation,
thereby resulting in prominence formation. Previous observational studies have
suggested that reconnection at a polarity inversion line of a coronal arcade
field creates a flux rope that can sustain a prominence; however, they did not
explain the origin of cool dense plasmas of prominences. Using
three-dimensional magnetohydrodynamic simulations including anisotropic
nonlinear thermal conduction and optically thin radiative cooling, we
demonstrate that reconnection can lead not only to flux rope formation but also
to radiative condensation under a certain condition. In our model, this
condition is described by the Field length, which is defined as the scale
length for thermal balance between radiative cooling and thermal conduction.
This critical condition depends weakly on the artificial background heating.
The extreme ultraviolet emissions synthesized with our simulation results have
good agreement with observational signatures reported in previous studies.

Solar and Stellar Astrophysics