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M. P. Ryutova (Lawrence Livermore National Laboratory/IGPP), T. D. Tarbell (Lockheed Martin Advanced Technology Center)
The spectra of CII and OVI lines corresponding to chromosphere and transition region temperatures show significant broadening and complex line profiles in regions overlying the sites of small scale magnetic elements in the photopsheric network. Doppler shifted multiple peaks in CII line are always seen soon after the reconnection of magnetic flux tubes occurs and usually consist of supersonic and subsonic components caused by shocks propagating upward. Multiple peaks in OVI line have more diverse features: they are not as persistent as those seen in CII line, and may have the configuration of maximum intensity peaks corresponding either to forward or reflected shocks. We develop a consistency analysis which allows to compare the shock relations and their properties with the observed signatures and infer physical parameters such as Mach number, direction of the shock propagation and velocities. We use the uninterrupted time series of data to trace particular events at the different stages of their evolution and deduce some intrinsic features of the mechanism of the energy production and its transport through the chromosphere/transition region.