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Space-borne missions CoRoT and {\it Kepler} are providing a rich harvest ofhigh-quality constraints on solar-like pulsators. Among the seismic parameters,mode damping rates remains poorly understood and thus barely used to inferphysical properties of stars. Nevertheless, thanks to CoRoT and {\it Kepler}space-crafts it is now possible to measure damping rates for hundreds ofmain-sequence and thousands of red-giant stars with an unprecedented precision.  By using a non-adiabatic pulsation code including a time-dependent convectiontreatment, we compute damping rates for stellar models representative forsolar-like pulsators from the main-sequence to the red-giant phase. This allowsus to reproduce the observations of both CoRoT and {\it Kepler}, whichvalidates our modeling of mode damping rates and thus the underlying physicalmechanisms included in the modeling. Actually, by considering the perturbationsof turbulent pressure and entropy (including perturbation of the dissipationrate of turbulent energy into heat) by the oscillation in our computation, wesucceed in reproducing the observed relation between damping rates andeffective temperature.  Moreover, we discuss the physical reasons for mode damping rates to scalewith effective temperature, as observationally exhibited. Finally, this opensthe way for the use of mode damping rates to probe turbulent convection insolar-like stars.

Damping rates of solar-like oscillations across the HR diagram. Theoretical calculations confronted to CoRoT and Kepler observations