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Limb darkening is an important stellar phenomenon and must be accounted forin the study of stellar spectra, eclipsing binaries, transiting planetarysystems, and microlensing events. The power-2 limb-darkening law provides agood match to the specific intensities predicted by stellar atmosphere models:it is better than other two-parameter laws and is only surpassed by thefour-parameter law. Predictions of the limb-darkening coefficients for thepower-2 law are not widely available. We therefore compute them, using stellaratmosphere models generated by the ATLAS (plane-parallel) code. Limb-darkeningcoefficients were computed for the space missions Gaia, Kepler, and TESS aswell as for the photometric systems uvby, UBVRIJHK, and SDSS ugriz.Thecalculations were performed by adopting the Levenberg-Marquardt least-squaresminimisation method and were computed with a resolution of 100 equally spacedviewing angles. We used 9586 model atmospheres covering 19 metallicities,effective temperatures of 3500 to 50000 K, log g values from 0.0 to 5.0, andmicroturbulent velocities of 0, 1, 2, 4, and 8 km. We confirm the superiorityof the power-2 law, in terms of the quality of the fits, over othertwo-parameter laws. This is particularly relevant for the quadratic law, whichis widely used. We recommend the use of the power-2 law in cases where atwo-parameter law is needed.

Power-2 limb-darkening coefficients for the uvby, UBVRIJHK, SDSS ugriz, Gaia, Kepler, and TESS photometric systems