Modelling of solar explosive events in 2D environments - III. Observable consequences

We examine the response via line synthesis of two representative transition region lines, namely C IV 1548.2 Angstrom and O VI 1031.9 Angstrom, in var ious physical environments representing the "quiet" Sun to magnetic reconne ction events. Our calculations of ion populations allow for departures from equilibrium ionization (EI), which is critical in studies of transient eve nts. Both lines reveal highly blue- and red-shifted Doppler components, and some of the results are examined in the context of solar explosive events. The observable consequences of magnetic reconnection are subtle in the var ious physical circumstances examined here and differ from one emission line to another, because of the difference in their formation temperatures.