- We compare hydrogen emission from 29 T Tauri stars with a grid 945 of synthetic line profiles.
- Our synthetic line profiles match the observed H⍺ widths, intensities and profile morphologies.
- However, our study indicates that reproducing H⍺, Paschen, and Brackett lines simultaneously is problematic. The synthetic infrared lines are too narrow and exhibit a higher than observed frequency of Inverse P-Cygni profiles.
Radiative Transfer Model - TORUS1
- Synthetic line profile computed using the radiative transfer code TORUS.
2.5D with adaptive mesh refinement
Atomic statistical equilibrium calculated for non-LTE. Sobolev with exact integration and pressure broadening
Co-moving frame ray-tracing
- Figure shows spectra of 29 T Tauri stars (columns) from the ESO Archive. The Stars are ordered by H⍺ intensity.
- Medium resolution (R~11600-18400) spectra from VLT’s X-Shooter, observed in Jan 2010.
- Near simultaneous observations of H⍺ (6562 Å), Pa𝛾 (10938 Å), Paβ (12818 Å), and Br𝛾 (21655 Å).
- A correlation of structure and intensity is seen between the infrared lines, this is not reflected by H⍺
- Reipurth classifications of the X-Shooter Observations (coloured bars) and the synthetic line profiles (hashed bars).
- Figure shows the FWHM vs. half width at 10% maxima (HW10%). Models are clipped so that H⍺ matches the observed HW10% range.
- Synthetic H⍺ lines reproduce well the observed range of widths and distribution of Reipurth types.
- The same models produce Pa𝛾, Paβ, and Br𝛾 lines ~70-100 kms-1 too narrow.
- Over 80% of the synthetic Pa𝛾, Paβ, and Br𝛾 lines exhibit Inverse P-Cygni profiles.
- Three examples of the best match between synthetic and observed H⍺ profiles.
- The models have been chosen because closely resemble the H⍺ obersvations in width and intensity.
- Despite the good H⍺ correspondence the infrared lines are poorly fitted.