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The amplitudes of solar-like oscillations depend on the excitation anddamping, both of which are controlled by convection. Comparing observationswith theory should therefore improve our understanding of the underlyingphysics. However, theoretical models invariably compute oscillation amplitudesrelative to the Sun, and it is therefore vital to have a good calibration ofthe solar amplitude using stellar techniques. We have used daytime spectra ofthe Sun, obtained with HARPS and UCLES, to measure the solar oscillations andmade a detailed comparison with observations using the BiSON helioseismologyinstrument. We find that the mean solar amplitude measured using stellartechniques, averaged over one full solar cycle, is 18.7 +/- 0.7 cm/s for thestrongest radial modes (l=0) and 25.2 +/- 0.9 cm/s for l=1. In addition, we usesimulations to establish an equation that estimates the uncertainty ofamplitude measurements that are made of other stars, given that the modelifetime is known. Finally, we also give amplitudes of solar-like oscillationsfor three stars that we measured from a series of short observations with HARPS(gamma Ser, beta Aql and alpha For), together with revised amplitudes for fiveother stars for which we have previously published results (alpha Cen A, alphaCen B, beta Hyi, nu Ind and delta Pav).

The amplitude of solar oscillations using stellar techniques