2018ApJ...866..153A

Non-local thermodynamical equilibrium (NLTE) line formation for Mg I and Mg II lines is considered in classical 1D LTE model atmospheres of the Sun and 17 stars with reliable atmospheric parameters and in a broad range of spectral types: 3900 K <= T_eff <= 17,500 K, 1.1 <= log g <= 4.7, and -2.6 <= [Fe/H] <= +0.4. We find that, for each star, NLTE leads to smaller line-to-line scatter. For 10 stars, NLTE leads to consistent abundances of Mg I and Mg II, while the difference in LTE abundance varies between -0.21 and +0.23 dex. We obtain an abundance discrepancy between Mg I and Mg II in two very metal-poor stars, HD 140283 and HD 84937. The origin of these abundance differences remains unclear. Our standard NLTE modeling predicts Mg I emission lines at 7.736, 11.789, 12.224, and 12.321 µm in the atmospheres with T_eff <= 7000 K. We reproduce well the Mg I 12.2 and 12.3 µm emission lines in Procyon. However, for the Sun and three K-giants, the predicted Mg I emission lines are too weak compared with the observations. For stars with 7000 K <= T_eff <= 17,500 K, we recommend the Mg II 3848, 3850, 4384, 4390, 4427, and 4433 Å lines for Mg abundance determinations even at the LTE assumption due to their small NLTE effects. The Mg I 4167, 4571, 4702, 5528, 5167, 5172, and 5183 Å lines can be safely used in the LTE analysis of stars with 7000 K < T_eff <= 8000 K. For the hotter stars, with T_eff from 8000 K to 9500 K, the NLTE effects are minor only for Mg I 4167, 4702, and 4528 Å.