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We have analyzed solar-like oscillations in ~1700 stars observed by theKepler Mission, spanning from the main-sequence to the red clump. Usingevolutionary models, we test asteroseismic scaling relations for the frequencyof maximum power (nu_max), the large frequency separation (Delta_nu) andoscillation amplitudes. We show that the difference of the Delta_nu-nu_maxrelation for unevolved and evolved stars can be explained by differentdistributions in effective temperature and stellar mass, in agreement with whatis expected from scaling relations. For oscillation amplitudes, we show thatneither (L/M)^s scaling nor the revised scaling relation by Kjeldsen & Bedding(2011) are accurate for red-giant stars, and demonstrate that a revised scalingrelation with a separate luminosity-mass dependence can be used to calculateamplitudes from the main-sequence to red-giants to a precision of ~25%. Theresiduals show an offset particularly for unevolved stars, suggesting that anadditional physical dependency is necessary to fully reproduce the observedamplitudes. We investigate correlations between amplitudes and stellaractivity, and find evidence that the effect of amplitude suppression is mostpronounced for subgiant stars. Finally, we test the location of the cool edgeof the instability strip in the Hertzsprung-Russell diagram using solar-likeoscillations and find the detections in the hottest stars compatible with adomain of hybrid stochastically excited and opacity driven pulsation.

Testing Scaling Relations for Solar-Like Oscillations from the Main Sequence to Red Giants using Kepler Data