The CHIANTI database has the following primary ASCII files for this ion:

- mg_11.elvlc (energy levels)
- mg_11.wgfa (radiative data)
- mg_11.scups (electron collision data)
- (proton collisional data) Not available in this VERSION.

contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

%filename: mg_11.elvlc Theoretical gf and A-values: Autostructure calculation A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE Badnell, N.R., 2011, Computer Physics Communications, 182, 1528 ADSref: http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B Observed energy levels (1s2s, 1s2p): Artemyev, A. N.; Shabaev, V. M.; Yerokhin, V. A.; Plunien, G.; Soff, G., 2005, Phys. Rev. A, 72, 2104 ADSref: http://adsabs.harvard.edu/abs/2005PhRvA..71f2104A %observed energy levels: Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 1995, NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61. Theoretical energies for n=2, 3 above IP Goryaev, F. F.; Vainshtein, L. A.; Urnov, A. M. Atomic data for doubly-excited states 2lnl of He-like ions and 1s2lnl of Li-like ions with Z = 6-36 and n = 2 , 3 2017, ADNDT, 113, 117-257 adsRef: http://adsabs.harvard.edu/abs/2017ADNDT.113..117G DOI: 10.1016/j.adt.2016.04.002 Theoretical energy levels (n=4,5 above IP): calculations of U. Safronova reported in Kato et al., 1997, ADNDT, 67, 225. ADS http://adsabs.harvard.edu/abs/1997ADNDT..67..225K updated by U. Safronova, 2001, private communication theoretical energy levels adjusted by SHFTIC file derived from Artemyev, Goryaev (n=2, 3 above IP) and Safronova (n= 4,5,6 above IP energies produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2020 June 19 mg_11 IP ev = 1.76180e+03 Ip invcm = 14209908.000 Ip Ryd = 129.49021 mg_12 IP ev = 1.96266e+03 Ip invcm = 15829955.000 Ip Ryd = 144.25316

contains wavelengths, gf and A values of the transitions. The wavelengths are based on the experimental energy levels and should be the best available. Wavelengths calculated from the theoretical energies are of an indeterminate accuracy and their values are presented as negative values of the calculated wavelength.

%filename: mg_11.wgfa.olg.imp Theoretical gf and A-values: Autostructure calculation A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE Badnell, N.R., 2011, Computer Physics Communications, 182, 1528 ADSref: http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B Observed energy levels (1s2s, 1s2p): Artemyev, A. N.; Shabaev, V. M.; Yerokhin, V. A.; Plunien, G.; Soff, G., 2005, Phys. Rev. A, 72, 2104 ADSref: http://adsabs.harvard.edu/abs/2005PhRvA..71f2104A %observed energy levels: Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 1995, NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61. Theoretical energies for n=2, 3 above IP Goryaev, F. F.; Vainshtein, L. A.; Urnov, A. M. Atomic data for doubly-excited states 2lnl of He-like ions and 1s2lnl of Li-like ions with Z = 6-36 and n = 2 , 3 2017, ADNDT, 113, 117-257 adsRef: http://adsabs.harvard.edu/abs/2017ADNDT.113..117G DOI: 10.1016/j.adt.2016.04.002 Theoretical energy levels (n=4,5 above IP): calculations of U. Safronova reported in Kato et al., 1997, ADNDT, 67, 225. ADS http://adsabs.harvard.edu/abs/1997ADNDT..67..225K updated by U. Safronova, 2001, private communication theoretical energy levels adjusted by SHFTIC file derived from Artemyev, Goryaev (n=2, 3 above IP) and Safronova (n= 4,5,6 above IP energies two-photon A-value: Derevianko, A.; Johnson, W. R., 1997, Phys Rev A, 56, 1288 Two-photon decay of 2 1S0 and 2 3S1 states of heliumlike ions ADSref: https://ui.adsabs.harvard.edu/abs/1997PhRvA..56.1288D/abstract wavelengths determined from energy levels minimum branching ratio = 1.00e-04 sorted by lvl12 elvlcName = mg_11.elvlc wgfaName = mg_11.wgfa-srt allWvl = 1 minDiff = 0.00010 outfile = mg_11.wgfa.olg.imp wavelengths determined from energy levels produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2020 June 19 %File processed with wgfa_tidy by pryoung on 31-May-2023

contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

K. Dere (GMU) - 2020 June 20 produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy collision strengths provided in the range 2.42e+04 to 2.42e+08 K DOI: http://dx.doi.org/10.1088/0953-4075/34/15/320 adsRef: http://adsabs.harvard.edu/abs/2001JPhB...34.3179W A radiation-dampedR-matrix approach to the electron-impact excitation of helium-like ions for diagnostic application to fusion and astrophysical plasmas Whiteford, A. D.; Badnell, N. R.; Ballance, C. P.; O'Mullane, M. G.; Summers, H. P.; Thomas, A. L. filename: mg_11.scups

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