Stellar limb darkening

The detection of the first exoplanet paved way into era transit photometry space missions with a revolutionary photometric precision that aim at discovering new exoplanetary systems around different types stars. With this high precision, it is possible to derive very accurately radii exoplanets which crucial for constraining their type and composition. However, requires an accurate description host stars, especially center-to-limb variation intensities (so called limb darkening) as affects planet-to-star radius ratio determination. We improving accuracy darkening calculations stars wide range fundamental parameters. used recently developed 1D MPS-ATLAS code compute model atmosphere structures synthesize stellar on fine grid For computations we utilized most information chemical element abundances mixing length parameters including convective overshoot. was fitted using two laws: power-2 4-parameters non-linear laws. present extensive library atmospheric structures, synthesized curves, coefficients parameterized limb-darkening laws in Kepler, TESS, CHEOPS, PLATO passbands. allows overcoming sizable errors introduced by need interpolate. Our solar are good agreement available measurements view angles wavelengths. agree well Kepler A broad filters provided CDS.