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The spin state of small asteroids can change on a long timescale by theYarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, the net torque that arisesfrom anisotropically scattered sunlight and proper thermal radiation from anirregularly-shaped asteroid. The secular change in the rotation period causedby the YORP effect can be detected by analysis of asteroid photometriclightcurves. We analyzed photometric lightcurves of near-Earth asteroids (1865)Cerberus, (2100) Ra-Shalom, and (3103) Eger with the aim to detect possibledeviations from the constant rotation caused by the YORP effect. We carried outnew photometric observations of the three asteroids, combined the newlightcurves with archived data, and used the lightcurve inversion method tomodel the asteroid shape, pole direction, and rotation rate. The YORP effectwas modeled as a linear change in the rotation rate in time d\omega /dt. Valuesof d\omega/ dt derived from observations were compared with the valuespredicted by theory. We derived physical models for all three asteroids. We hadto model Eger as a nonconvex body because the convex model failed to fit thelightcurves observed at high phase angles. We probably detected theacceleration of the rotation rate of Eger d\omega / dt = (1.4 +/- 0.6) x10^{-8} rad/d (3\sigma error), which corresponds to a decrease in the rotationperiod by 4.2 ms/yr. The photometry of Cerberus and Ra-Shalom was consistentwith a constant-period model, and no secular change in the spin rate wasdetected. We could only constrain maximum values of |d\omega / dt| < 8 x10^{-9} rad/d for Cerberus, and |d\omega / dt| < 3 x 10^{-8} rad/d forRa-Shalom.

Analysis of the rotation period of asteroids (1865) Cerberus, (2100) Ra-Shalom, and (3103) Eger - search for the YORP effect