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Results of calculations for inelastic e+Mg effective collision strengths forthe lowest 25 physical states of Mg I (up to 3s6p 1P), and thus 300transitions, from the convergent close-coupling (CCC) and the B-spline R-matrix(BSR) methods are presented. At temperatures of interest, ~5000 K, the resultsof the two calculations differ on average by only 4%, with a scatter of 27%. Asthe methods are independent, this suggests that the calculations providedatasets for e+Mg collisions accurate to this level. Comparison with thecommonly used dataset compiled by Mauas et al. (1988), covering 25 transitionsamong 12 states, suggests the Mauas et al. data are on average ~57% too low,and with a very large scatter of a factor of ~6.5. In particular the collisionstrength for the transition corresponding to the Mg I intercombination line at457 nm is significantly underestimated by Mauas et al., which has consequencesfor models that employ this dataset. In giant stars the new data leads to astronger line compared to previous non-LTE calculations, and thus a reductionin the non-LTE abundance correction by ~0.1 dex (~25%). A non-LTE calculationin a supernova ejecta model shows this line becomes significantly stronger, bya factor of around two, alleviating the discrepancy where the 457 nm line intypical models with Mg/O ratios close to solar tended to be too weak comparedto observations.

Inelastic e+Mg collision data and its impact on modelling stellar and supernova spectra