Atomic data and spectral line intensities for Mg V
Abstract
Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Mg V. The configurations used are 2s^{2}2p^{4}, 2s2p^{5}, 2p^{6}, 2s^{2}2p^{3}3s, 2s^{2}2p^{3}3p, and 2s^{2}2p^{3}3d, giving rise to 86 finestructure levels in intermediate coupling. Collision strengths are calculated at five incident energies, 10, 20, 30, 40, and 50 Ry, in the distorted wave approximation. Excitation rate coefficients (not tabulated here) are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. To calculate excitation rate coefficients, collision strengths at low and high energy limits are calculated by a method described by Burgess and Tully. Using the excitation rate coefficients and the radiative transition rates, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10^{8} 10^{14} cm^{3} at an electron temperature of log T_{e} = 5.4, corresponding to the maximum abundance of Mg V. Fractional level populations and relative spectral line intensities are also calculated. Our calculated intensities are compared with the active region observations from the solar EUV rocket telescope and spectrograph (SERTS) and the diagnostic properties of Mg V are discussed. This dataset will be made available in the next version of the CHIANTI database.
 Publication:

Atomic Data and Nuclear Data Tables
 Pub Date:
 January 2006
 DOI:
 10.1016/j.adt.2005.09.002
 Bibcode:
 2006ADNDT..92..105B