Table E.1.
Configuration of TARDIS simulations used to fit the measured spectra with the synthesized spectra.
| Constant parameters of TARDIS simulations | |||
|---|---|---|---|
| Atomic physics database: | Monte-Carlo settings: | ||
| atom_data: | kurucz_cd23_chianti_H_He.h5 | montecarlo: | |
| Model settings: | seed: | 10000000 | |
| model: | no_of_packets: | 50000 | |
| structure: | iterations: | 20 | |
| type: | file | last_no_of_packets: | 150000 |
| filename: | density.dat | no_of_virtual_packets: | 4 |
| filetype: | simple_ascii | convergence_strategy: | |
| abundances: | type: | damped | |
| type: | file | damping_constant: | 1.0 |
| filename: | abundance.dat | threshold: | 0.05 |
| filetype: | custom_composition | fraction: | 0.8 |
| Plasma configuration: | hold_iterations: | 3 | |
| plasma: | t_inner_update_exponent: | -0.5 | |
| ionization: | nebular | t_inner: | |
| excitation: | dilute-lte | damping_constant: | 1.0 |
| radiative_rates_type: | dilute-blackbody | threshold: | 0.05 |
| line_interaction_type: | macroatom | t_rad: | |
| disable_electron_scattering: | False | damping_constant: | 1.0 |
| disable_line_scattering: | False | threshold: | 0.05 |
| nlte: | w: | ||
| species: | [] | damping_constant: | 1.0 |
| coronal_approximation: | False | threshold: | 0.05 |
| classical_nebular: | False | Spectrum settings: | |
| continuum_interaction: | spectrum: | ||
| species: | [] | start: | 1700 angstrom |
| enable_adiabatic_cooling: | False | stop: | 10000 angstrom |
| enable_two_photon_decay: | False | num: | 600 |
| helium_treatment: | none | ||
| link_t_rad_t_electron: | 0.9 | ||
Notes. From top to bottom, the blocks are as follows: 1) The database used for atomic and statistical physics calculations. 2) The TARDIS model settings: the density and abundance profile are taken from an external data file, enabling their cell-by-cell definition. It is important to note that while the data in this table remains constant, the actual content of the mentioned files, i.e., the density and abundance profile, serves as fitting parameters in the simulations. The details are discussed in Section 5. 3) Settings related to plasma calculations 4) Parameters for Monte Carlo iterations and the update of various physical quantities per iteration. The quantities indexed with ’inner’ refer to the photosphere. 5) The last block contains settings related to the synthesized spectrum.
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