Line ModelsHere you can find output from the models of H I line emission developed by John Kwan and presented in our 2011 paper. If you use these, please cite Kwan, J., & Fischer, W. 2011, MNRAS, 411, 2383.
View the ADS list of citations to the paper for examples of how the models have been used.
The results are expressed as the ratios of various lines to Pa β for a range of densities and temperatures. We include lower levels from 2 to 7 and upper levels up to 20. Each file contains ratios for a given line; the naming convention is upper-lower_pabeta.txt. Ratios are for 23 densities shown in the first column (log cm−3) and for seven temperatures shown in the column headings (K).
Results are presented for three cases.
Cases 1 and 2 feature photoionization of the excited states via a stellar continuum, assumed to be a 4000 K blackbody, and a veiling continuum, assumed to be an 8000 K blackbody covering 3% of the stellar surface.
Case 3 is primarily illustrative in nature. For other cases, if information is available on the velocity gradient (i.e., the physical size and velocity span of the emission region) and any incident ionization source, new calculations can be requested by emailing me (W. Fischer; see a recent first-author paper for my address).
|Case||Example Application||Density Range (log cm−3)||Temperature Range (K)||Photoionization Rate from Ground State (s−1)||Velocity Gradient||Files|
|I1||T Tauri stars||8.0 – 12.4||3750 – 15000||2×10−4||300 km s−1 / 8 R☉||Case I|
|II||T Tauri stars||8.0 – 12.4||3750 – 15000||2×10−6||300 km s−1 / 8 R☉||Case II|
|III||Novae||8.0 – 12.4||7500 – 20000||0||300 km s−1 / 1000 R☉||Case III|