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Published February 16, 2009 | Published
Book Section - Chapter Open

A Consistent Model of the Accretion Shock Region in Classical T Tauri Stars

Abstract

We develop a consistent model of the accretion shock region in Classical T Tauri Stars (CTTSs). The initial conditions of the post-shock flow are determined by the irradiated shock precursor and the ionization state is calculated without assuming ionization equilibrium. Comparison with observations of the C IV resonance lines (λλ 1550 Å) for CTTSs indicate that the post-shock emission predicted by the model is too large, for a reasonable range of parameters. If the model is to reproduce the observations, C IV emission from CTTSs has to be dominated by pre-shock emission, for stars with moderate to large accretion rates. For stars with low accretion rates, the observations suggest a comparable contribution between the pre- and post-shock regions. These conclusions are consistent with previous results indicating that the post-shock will be buried under the stellar photosphere for moderate to large accretion rates.

Additional Information

© 2009 American Institute of Physics. Calculations of the pre-shock structure were performed with version 07.02.00 of Cloudy [4]. Calculations of the post-shock structure were performed with CHIANTI v.5.2.1. CHIANTI is a collaborative project involving the NRL (USA), RAL (UK), and the following Univerisities: College London (UK), Cambridge (UK), George Mason (USA), and Florence (Italy).

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August 21, 2023
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