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The larger number of models of asteroid shapes and their rotational statesderived by the lightcurve inversion give us better insight into both the natureof individual objects and the whole asteroid population. With a largerstatistical sample we can study the physical properties of asteroidpopulations, such as main-belt asteroids or individual asteroid families, inmore detail. Shape models can also be used in combination with other types ofobservational data (IR, adaptive optics images, stellar occultations), e.g., todetermine sizes and thermal properties. We use all available photometric dataof asteroids to derive their physical models by the lightcurve inversion methodand compare the observed pole latitude distributions of all asteroids withknown convex shape models with the simulated pole latitude distributions. Weused classical dense photometric lightcurves from several sources andsparse-in-time photometry from the U.S. Naval Observatory in Flagstaff,Catalina Sky Survey, and La Palma surveys (IAU codes 689, 703, 950) in thelightcurve inversion method to determine asteroid convex models and theirrotational states. We also extended a simple dynamical model for the spinevolution of asteroids used in our previous paper. We present 119 new asteroidmodels derived from combined dense and sparse-in-time photometry. We discussthe reliability of asteroid shape models derived only from Catalina Sky Surveydata (IAU code 703) and present 20 such models. By using different values for ascaling parameter cYORP (corresponds to the magnitude of the YORP momentum) inthe dynamical model for the spin evolution and by comparing synthetics andobserved pole-latitude distributions, we were able to constrain the typicalvalues of the cYORP parameter as between 0.05 and 0.6.

Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution