Accretion shock on CTTSs and its X-ray emission
Abstract
High spectral resolution X-ray observations of classical T Tauri stars (CTTSs) demonstrate the presence of plasma at T~2-3×106 K and ne~1011-1013 cm-3. Stationary models suggest that this emission is due to shock-heated accreting material. We address this issue by a 1-D hydrodynamic model of the impact of the accretion flow onto a chromosphere of a CTTS with the aim of investigating the stability of accretion shock and the role of the chromosphere. Our simulations include the effects of gravity, radiative losses from optically thin plasma, the thermal conduction and a detailed modeling of the stellar chromosphere. Here we present the results of a simulation based on the parameters of the CTTS MP Mus.
- Publication:
-
15th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun
- Pub Date:
- February 2009
- DOI:
- 10.1063/1.3099112
- Bibcode:
- 2009AIPC.1094..329S
- Keywords:
-
- 96.50.Fm;
- 78.70.En;
- 02.60.-x;
- 95.30.Lz;
- Planetary bow shocks;
- interplanetary shocks;
- X-ray emission spectra and fluorescence;
- Numerical approximation and analysis;
- Hydrodynamics;
- shock waves;
- X-ray emission spectra;
- numerical analysis;
- hydrodynamics