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We present sensitive and high angular resolution ($\sim$0.2-0.3$''$)(sub)millimeter (230 and 345 GHz) continuum and CO(2$-$1)/CO(3$-$2) linearchive observations of the disk star system in UX Tauri carried out with ALMA(The Atacama Large Millimeter/Submillimeter Array). These observations revealthe gas and dusty disk surrounding the young star UX Tauri A with a largesignal-to-noise ratio ($>$400 in the continuum and $>$50 in the line), and forthe first time is detected the molecular gas emission associated with the diskof UX Tauri C (with a size for the disk of $<$56 au). No (sub)millimetercontinuum emission is detected at 5$\sigma$-level (0.2 mJy at 0.85 mm)associated with UX Tauri C. For the component UX Tauri C, we estimate a dustdisk mass of $\leq$ 0.05 M$_\oplus$. Additionally, we report a strong tidaldisk interaction between both disks UX Tauri A/C, separated 360 au in projecteddistance. The CO line observations reveal marked spiral arms in the disk of UXTauri A and an extended redshifted stream of gas associated with the UX Tauri Cdisk. No spiral arms are observed in the dust continuum emission of UX Tauri A.Assuming a Keplerian rotation we estimate the enclosed masses (disk$+$star)from their radial velocities in 1.4 $\pm$ 0.6 M$_\odot$ for UX Tauri A, and 70$\pm$ 30 / $\sin i$ Jupiter masses for UX Tauri C (the latter coincides withthe mass upper limit value for a brown dwarf). The observational evidencepresented here lead us to propose that UX Tauri C is having a close approach ofa possible wide, evolving and eccentric orbit around the disk of UX Tauri Acausing the formation of spiral arms and the stream of molecular gas fallingtowards UX Tauri C.

Tidal Interaction between the UX Tauri Disk A/C System Revealed by ALMA