  Prominences and coronal rain are two forms of coronal condensations for which
we still lack satisfactory details on the formation pathways and conditions
under which the two come to exist. We compared prominences that formed via a
steady versus stochastic type of heating. We performed 2.5D simulations using
the open-source MPI-AMRVAC code. To further extend the work and allow for
future direct comparison with observations, we used Lightweaver to form spectra
of the filament view of our steady case prominence. With that, we analysed a
reconnection event that shares certain characteristics with nanojets. We show
how different forms of localised heating that induce thermal instability result
in prominences with different properties. The steady form of heating results in
prominence with a clear vertical structure stretching across the magnetic field
lines. On the other hand, stochastic heating produces many threads that
predominantly have a horizontal motion along the field lines. In the steady
heating case, the prominence is relatively static; however, there is evidence
of reconnection happening almost the entire time the prominence is present. In
the case of stochastic heating, the threads are highly dynamic, with them also
exhibiting a form of transverse oscillation (strongly resembling the decayless
type). The fact that the threads in the stochastic heating case are constantly
moving along the field lines suppresses any conditions for reconnection. It,
therefore, appears that, to first order, the choice of heating prescription
defines whether the prominence-internal dynamics are oriented vertically or
horizontally. We closely inspected a sample reconnection event and computed the
synthetic optically thick radiation using the open-source Lightweaver radiative
transfer framework.
