SASSO, CLEMENTINACLEMENTINASASSOANDRETTA, VincenzoVincenzoANDRETTATERRANEGRA, LucianoLucianoTERRANEGRAGomez, Maria TeresaMaria TeresaGomez2020-09-032020-09-0320170004-6361http://hdl.handle.net/20.500.12386/27076Context. The Mg I 4571 Å line and the b triplet are denoted in the literature as diagnostics of solar and stellar activity since their formation is in the low chromosphere. Aims: We aim to investigate the potential of these four spectral lines as diagnostics of chromospheric activity in solar-like stars, studying the dependence of the intensity of these lines from local atmospheric changes by varying atmospheric models and stellar parameters. <BR /> Methods: Starting with Next-Gen photospheric models, we build a grid of atmospheric models including photosphere, chromosphere and transition region and solve the radiative transfer to obtain synthetic profiles to compare with observed spectra of main-sequence, solar like stars with effective temperatures in the range 4800-6400 K, solar gravity and solar metallicity. Results: We find that the Mg I 4571 Å line is significantly sensitive to local changes in the atmospheric model around the minimum temperature. Conversely, the lines of the b triplet do not show significant responses to changes on the local atmospheric structure.STAMPAenArticle10.1051/0004-6361/2017306762-s2.0-85026829988000408480100093https://www.aanda.org/articles/aa/abs/2017/08/aa30676-17/aa30676-17.html2017A&A...604A..50SFIS/05 - ASTRONOMIA E ASTROFISICA