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The correct interpretation of the large amount of complex data fromnext-generation (in particular, space-based) observational facilities requiresa very strong theoretical underpinning. One can thus predict that in the nearfuture the use of atmospheric models obtained through the use ofthree-dimensional (3-D) radiation magnetohydrodynamics (RMHD) codes, coupledwith advanced radiative transfer treatment including non-local thermodynamicequilibrium (non-LTE) effects and polarisation, will become the norm. Inparticular, stellar brightness variability in cool (i. e., spectral type F, G,K, and M) stars can be induced by several different effects, besides pulsation.We briefly discuss some literature results and mention some of our recentprogress. Finally, we attempt to peek into the future of understanding thisimportant aspect of the life of stars.

Shine BRITE: shedding light on stellar variability through advanced models