Variability in the Gas and Dust Emission of the UX Orioni Star CQ Tau

UX Orionis type stars are intermediate-mass pre-main-sequence stars that are distinguished from other pre-main-sequence stars by their large photometric and polarimetric variations that are thought to be due to variable extinction by circumstellar dust. CQ Tau has been classified as a UX Orioni type star by several authors. In this paper, we aim to present different physical scenarios where the photometric variability of CQ Tau can be described. We propose that the variability in gas and dust emission can take place due to physical phenomena at different positions in the disk allowing for the obscuration in the photometric data to occur depending on when observed.