Other
Scientific paper
Jul 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992hst..prop.3845b&link_type=abstract
HST Proposal ID #3845
Other
Hst Proposal Id #3845
Scientific paper
Currently there is complete confusion as to the physical origin of the UV emission lines in T Tauri stars, although they are the strongest known UV emissions from cool stars. Possibilities include closed magnetic field loops in analogy to active main sequence stars, a hot region in an Alfven wind, the accretion boundary layer between star and disk, accretion columns in the stellar magnetic field, or some other region associated with a disk-generated wind. Emission measure analyses have been unable to distinguish between the possibilities listed above. What is clearly needed is line profile information: in particular a good measurement of the breadth of the profiles and a reasonable idea of their symmetry. Narrow lines will indicate plasma originating either on the stellar surface or in closed magnetic loops. Broad lines will indicate a turbulent boundary layer or wind region. The asymmetry of the lines will indicate whether they arise in accretion, outflow, or relatively static plasma, and something about the size of the region (via occulation effects). Taken with some emission measures, density diagnostics, and wind diagnostic information, the current mystery about the origin of these strong hot emission lines can be illuminated. We propose to measure enough profiles and emission measures in a representative small sample of stars to constrain, support or eliminate the above hypotheses.
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