Accretion Shocks in Classical T-Tauri Stars

Details Accretion Shocks in Classical T-Tauri Stars Accretion Shocks in Classical T-Tauri Stars

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9933j&link_type=abstract

HST Proposal ID #9933

Physics

Hst Proposal Id #9933 Star Formation

Scientific paper

We will develop a model of the accretion shock region of Classical T-Tauri stars. The goal of the model is to relate the observed strong ultraviolet emission in transition region lines {the SiIV resonance doublets, the CIV resonance doublets, etc} seen with HST-GHRS and HST-STIS to the physical parameters that control the accretion process {accretion rate, size of accretion region, topology of magnetic field, etc.} Current analysis of the transition region lines {which are important components of HST UV spectral observations of Classical T-Tauris} is limited by the lack of complete published models. The accretion shock region is composed of a post-shock region, and a ionized precursor, or pre-shock. Modeling of the former will take into account that the emiting gas is not in ionization equilibrium, and that its emission affects the pre-shock, which in turn determines the initial conditions of the post-shock. The pre-shock will be modeled with a photoionization code.

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