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Based on multiyear INTEGRAL observations of SS433 in 2003-2011, a compositeIBIS/ISGRI 18-60 keV orbital light curve is constructed around zeroprecessional phases psi_{pr}= 0 at the maximim accretion disk opening angle. Itshows a peculiar shape with significant excess near the orbital phase phi_orb=0.25, which is not seen in the softer 2-10 keV energy band. The 40-60 keVorbital light curve demonstrates two almost equal humps at phases \sim 0.25 and\sim 0.75, most likely due to nutation effects of the accretion disk. Thenutational variability of SS433 in 15-50 keV with a period of 6.290 days isindependently found from timing analysis of Swift/BAT data. The change of theoff-eclipse 18-60 keV X-ray flux with the precessional phase shows adouble-wave form with strong primary maximum at psi_{pr}= 0 and weak butsignificant secondary maximum at psi_{pr}= 0.6. A weak variability of the 18-60keV flux in the middle of the orbital eclipse correlated with the diskprecessional phase is also observed. The joint analysis of the broadband 18-60keV orbital and precessional light curves confirms the presence of a hotextended corona in the central parts of the supercritical accretion disk andconstrains the binary mass ratio in SS433 in the range 0.5>q>0.3, suggestingthe black hole nature of the compact object.

INTEGRAL observations of SS433: system's parameters and nutation of supercritical accretion disk