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The study of spiral structures in protoplanetary disks is of great importancefor understanding of processes in the disks, including planet formation. Brightspiral arms were detected in the disk of young star CQ Tau by Uyama et al.(2020) in H and L bands. The spiral arms are located inside the gap inmillimeter size dust, recovered earlier using ALMA observations (UbeiraGabellini et al. 2019). To explain the gap, Ubeira Gabellini et al. (2019)proposed the existence of a planet with the semimajor axis of 20 AU. Weobtained multiepoch observations of a spiral feature in the circumstellarenvelope of CQ Tau in Ic band using a novel technique of differential specklepolarimetry. The observations covering period from 2015 to 2021 allow us toestimate the pattern speed of spiral: $-0.2\pm1.1^{\circ}$/yr (68% credibleinterval, positive value indicates counter-clockwise rotation), assumingface-on orientation of the disk. This speed is significantly smaller thanexpected for a companion-induced spiral, if the perturbing body has thesemimajor axis of 20 AU. We emphasize that the morphology of the spiralstructure is likely to be strongly affected by shadows of a misaligned innerdisk detected by Eisner et al. (2004).

Apparent motion of the circumstellar envelope of CQ Tau in scattered light