Computer Science
Scientific paper
Jul 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8132r&link_type=abstract
HST Proposal ID #8132
Computer Science
Hst Proposal Id #8132 Young Stars And Circumstellar Material
Scientific paper
The forbidden line emission, of what are probably the youngest classical T Tauri stars and Herbig Ae/Be stars, is often characterised by two radial velocity components. The so-called high velocity component {HVC} is thought to be a jet close to the source since its velocity is normally found to coincide with that of any associated, and extended, Herbig-Haro type jet. In comparison very little is known about the low velocity component {LVC}. In this study, we will carry out a detailed investigation of the outflows from the classical T Tauri star RW Aur and the Herbig Ae/Be star LkHAlpha 233 using long-slit spectroscopic imaging. This technique will provide both 2-D intensity and radial velocity data for the HVC and LVC of these flows. Our targets are ideal in that there is very little extinction towards either of these young stellar objects {YSOs} thereby allowing us to study the morphology and dynamics of the innermost regions {<= 1''} of their outflows. The observations wil l be used to address a number of fundamental questions that are common to outflows from both low and intermediate mass young stars. What, for example, is the origin of the LVC, which is much more compact {<= 1''} than the jet? The LVC is often neglected in outflow models although it may be some form of poorly collimated disk wind. To test this idea, the superior resolution of the HST is required. What is the velocity, temperature, ionization fraction and density of these flows on scales of 0.1''-2'? Can we find evidence for entrainment and velocity variations close to the source? Finally by spectroscopically imaging along the extended outflow {jet} direction, we should also be able to examine, for example, what the transverse velocity profile of a YSO jet looks like. Is there evidence for an extensive boundary layer? How do the fundamental parameters mentioned above, such as ionization fraction, change along the jet?
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