A Consistent Model of the Accretion Shock Region in Classical T Tauri Stars
- Creators
- Ardila, D. R.
- Johns-Krull, C. M.
- Other:
- Stempels, Eric
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).Attached Files
Published - Ardila2009p8151Cool_Stars_Stellar_Systems_And_The_Sun.pdf
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Additional details
- Eprint ID
- 18222
- Resolver ID
- CaltechAUTHORS:20100510-142047910
- Created
-
2010-06-01Created from EPrint's datestamp field
- Updated
-
2021-11-08Created from EPrint's last_modified field
- Series Name
- AIP Conference Proceedings
- Series Volume or Issue Number
- 1094