Description
Transition probabilities and electron impact excitation collision strengths and rates for astrophysically important lines in Mg V are reported. The 86 fine-structure levels of the 2s^2^2p^4^, 2s2p^5^, 2p^6^, 2s2^2^p^3^3s, 2s^2^2p^3^3p and 2s^2^2p^3^3d configurations are included in our calculations. The effective collision strengths are presented as a function of electron temperature for solar and other astrophysical applications.
|