The following document lists the file abstract/MSMITH_COBOW.abs
from catalogue VI/111.
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===================================================================== ==> In this proposal, more time is being requested for MSMITH.RALEINAD ===================================================================== Very young protostars, even though deeply embedded, can still be observed at infrared wavelengths. The discovered outflows, amazing for there ubiquity, collimation and power, occur during a phase in which inflow was thought to dominate. The outflows drive complex shock structures. To understand the shocks, we are developing a full program to suppliment our ground-based studies of the hot molecular hydrogen. We plan to use the full set of diagnostics on the molecular gas. Thus, the SWS will attempt to observe pure-rotational lines in vibrationally-excited H2 (RALEINAD). We have also made definite predictions for the cooler gas from the bow shocks, including the high-J CO transitions in the LWS range. This cool gas exists in three distinct areas: in the same post-shock gas, deep in the bow flanks or in the supersonic turbulence created behind curved shock fronts. Thus we now propose to study these transitions in the outflow HH211, which possesses many curved shock structures. We demonstrate here how we would use this data to learn more about outflow physics, including the more general star-formation problem of the dissipation of supersonic turbulence.