  We report VLBI monitoring observations of the 22 GHz water (H$_{2}$O) masers
around the Mira variable BX Cam, which were carried out as a part of the EAVN
Synthesis of Stellar Maser Animations (ESTEMA) project. Data of 37 epochs in
total were obtained from 2018 May to 2021 June with a time interval of 3-4
weeks, spanning approximately three stellar pulsation periods ($P= \sim$440 d).
In particular, the dual-beam system equipped on the VERA stations was used to
measure the kinematics and parallaxes of the H$_{2}$O maser features. The
measured parallax, $\pi=1.79\pm 0.08$ mas, is consistent with $Gaia$ EDR3 and
previously measured VLBI parallaxes within a 1-$\sigma$ error level. The
position of the central star was estimated, based on both the $Gaia$ EDR3 data
and the center position of the ring-like 43 GHz silicon-monoxide (SiO) maser
distribution imaged with the KVN. The three-dimensional H$_{2}$O maser
kinematics indicates that the circumstellar envelope is expanding at a velocity
of $13\pm4$ km s$^{-1}$, while there are asymmetries in both the spatial and
velocity distributions of the maser features. Furthermore, the H$_{2}$O maser
animation achieved by our dense monitoring program manifests the propagation of
shock waves in the circumstellar envelope of BX Cam.
