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A significant fraction of the envelope of low- and intermediate-mass stars isunstable to convection, leading to sub-surface turbulent motion. Here, weconsider and include the effects of turbulence pressure in our stellarevolution calculations. In search of an observational signature, we compare thefractional contribution of turbulent pressure to the observed macroturbulentvelocities in stars at different evolutionary stages. We find a strongcorrelation between the two quantities, similar to what was previously foundfor massive OB stars. We therefore argue that turbulent pressure fluctuationsof finite amplitude may excite high-order, high-angular degree stellaroscillations, which manifest themselves at the surface an additional broadeningof the spectral lines, i.e., macroturbulence, across most of the HR diagram.When considering the locations in the HR diagram where we expect high-orderoscillations to be excited by stochastic turbulent pressure fluctuations, wefind a close match with the observational $\gamma$ Doradus instability strip,which indeed contains high-order, non-radial pulsators. We suggest thatturbulent pressure fluctuations on a percentual level may contribute to the$\gamma$ Dor phenomenon, calling for more detailed theoretical modelling inthis direction.

Relating turbulent pressure and macroturbulence across the HR diagram with a possible link to \gamma-Dor stars