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Scientific paper
Jul 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8628g&link_type=abstract
HST Proposal ID #8628
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Hst Proposal Id #8628 Star Formation
Scientific paper
Outflow is ubiquotous during star formation however the mechanism which drives it, is still uknown. The key observational information about how outflow is initiated is contained within a region of angular size smaller than 0.1 arcsec {for the nearest stars} which is not accessible to direct imaging. It has been shown that the jet density increases towards the source but the commonly used optical forbidden lines cannot probe densities higher than 10^6 cm^- 3. An analysis of the ultraviolet tracers of shocked material carried out by us and based on data from the HST Archive has shown that jet emission is also detected from the UV semiforbidden lines of CIII]{1908 A} and SiIII]{1892 A}. The infered electronic density of the emitting gas is 1e9 - 1e10 cm-3. Therefore the UV semiforbidden lines provide a unique tool for studying the physics of jet formation within the ``black box'' which is not accessible by other means. This project, however, can only be carried out with: HST+STIS. Given the relevance of studying the base of the jet to understand the physics of outflow {and accretion} in star formation, we apply in this proposal for HST observing time to measure the CIII] and SiIII] lines in a small sample of T Tauri stars. Our objective is to compare the kinematics of the UV line formation region with that of the optical forbidden lines and to determine the physical characteristics of the jet formation region.
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