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We present the latest and final version of the movie of the SiO masers towardthe Mira variable TX Cam. The new version consists of 112 frames (78successfully reduced epochs) with data covering almost three complete stellarcycles between 24 May 1997 to 25 January 2002, observed with the VLBA. In thispaper we examine the global morphology, kinematics and variability of themasering zone. The morphology of the emission is confined in a structure thatusually resembles a ring or an ellipse, with occasional deviations due tolocalised phenomena. The ring appears to be contracting and expanding, althoughfor the first cycle contraction is not observed. The width and outer boundaryof the masering zone follow the stellar pulsation. Our data seem to beconsistent with a shock being created once per stellar cycle at maximum thatpropagates with a velocity of ~7 km/s. The difference in velocities alongdifferent axes strongly suggests that the outflow in TX Cam is bipolar. Thecontribution of projection is examined and our results are compared with thelatest theoretical model.

A long-term VLBA monitoring campaign of the v=1, J=1-0 SiO masers toward TX Cam - I. Morphology and Shock Waves