The following document lists the file abstract/DJAFFE_LVS.abs
from catalogue VI/111.
A plain copy of the file
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The goals of this proposal are to characterize the physical nature and emergent spectrum of low velocity (v<15-20 km/sec) shocks in the dense interstellar medium and to test models of MHD shocks in the low velocity range where they are hitherto untested. High velocity MHD shocks from protostellar outflows, Herbig-Haro objects, and supernova remnants have been studied extensively from the ground in optical and IR lines. There are already good plans for studies of such objects in the ISO Central Program. There is no corresponding plan to study low velocity shocks. Low velocity shocks are important as signposts of injection and dissipation of turbulent energy in the dense ISM. We expect to see emission from such shocks in three contexts: swept-up or entrained gas in protostellar flows, gas shocked ahead of HII ionization fronts, and clouds with high velocity dispersions. The first two represent possible sources for injection of kinetic energy into clouds. The third type of shock may be a result of dissipation of internal motion. We will examine a small sample of protostellar flows and turbulent clouds in the OI 63 micron line and several ground state rotational transitions of H2. The targets have been chosen to avoid regions with high velocity shocks or strong PDR emission. We will test for PDR contamination with CII observations and ground-based H2 observations.