Synthesis of optically thin emission line and continuum spectra for solar and stellar coronae for the non-Maxwellian kappa-distributions.
Currently, the software and database allows calculation of the synthetic spectra for kappa = 2, 3, 4, 5, 7, 10, 15, 25, and 33.
Corresponding Maxwellian spectra can be calculated using CHIANTI, version 10 and 9
(Dere, K.P. . Del Zanna, G. Young, P.R., Landi, E., Sutherland, R. S.: 1997, Astrophys. J. Suppl. Ser., 241, 22;
Del Zanna, G., Dere, K.P., Young, P.R., Landi, E.: 2021, Astrophys. J. 909, 38)
or using Maxwellian branche of KAPPA package.
1) CHIANTI 10 is required
2) Copy the files and database into a standalone folder kappa/
3) The '!data_pth' system variable has to be set, pointing to the directory with the database (including full path)
EXAMPLE:
defsysv, '!data_pth', '/home/user/kappa/data'
EXAMPLES:
.r /home/user/kappa/ch_load_2ion_rates_k.pro
.r /home/user/kappa/ch_load_ion_rates_k.pro
.r /home/user/kappa/ch_setup_ion_k.pro
.r /home/user/kappa/ch_synthetic_k.pro
.r /home/user/kappa/descale_diel_k.pro
.r /home/user/kappa/emiss_calc_k.pro
.r /home/user/kappa/freebound_k.pro
.r /home/user/kappa/freebound_ion_k.pro
.r /home/user/kappa/freefree_k.pro
.r /home/user/kappa/freefree_k_integral.pro
.r /home/user/kappa/isothermal_k.pro
.r /home/user/kappa/kappa.pro
.r /home/user/kappa/make_kappa_spec_k.pro
.r /home/user/kappa/plot_populations_k.pro
.r /home/user/kappa/pop_solver_k.pro
.r /home/user/kappa/read_ff_k.pro
.r /home/user/kappa/read_ionrec_k.pro
.r /home/user/kappa/read_rate_ioniz_k.pro
.r /home/user/kappa/read_rate_recomb_k.pro
.r /home/user/kappa/read_kappa_ups.pro
.r /home/user/kappa/ups_kappa_interp.pro
....
The above examples can be included into the idl_startup.pro for automatic compilation.
The routines above contain as the first parameter a value of kappa with the exception of the main widget routine kappa.pro where parameter kappa is given by the selection of the ionization equilibrium.
EXAMPLES:
kappa_02.ioneq - calculations for kappa=2
chianti.ioneq - calculations for the Maxwellian distribution
Last update: August 8, 2022
This work was supported by Grant Agency of the Czech Republic, Grant No. 18-09072S. We acknowledge the CHIANTI database and software, www.chiantidatabase.org, on which the KAPPA package is based and without which it could not exist. CHIANTI is a collaborative project involving the NRL (USA), RAL (UK), MSSL (UK), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). It is a great spectroscopic database and software and the authors are very grateful for its existence and availability.