  New analyses of earlier ALMA observations of oxygen-rich AGB star EP Aquarii
are presented, which contribute major progress to our understanding of the
morpho-kinematics of the circumstellar envelope (CSE). The birth of the
equatorial density enhancement (EDE) is shown to occur very close to the star
where evidence for rotation has been obtained. High Doppler velocity wings are
seen to consist of two components, the front end of the global wind, reaching
above $\pm$12 \kms, and an effective line broadening, confined within 200 mas
from the centre of the star, reaching above $\pm$20 \kms\ and interpreted as
caused by the pattern of shock waves resulting from the interaction between
stellar pulsation and convective cell granulation. Close to the star, episodic
and lumpy mass ejections are observed, and their interaction with the gas of
the nascent EDE, first rotating and later slowly expanding, is seen to play an
important role in the development of the wind and the evolution of its radial
velocity from 8-10 \kms\ on the polar symmetry axis to $\sim$2 \kms\ at the
equator. It implies a very complex morpho-kinematics, which prevents making
reliable interpretations with reasonable confidence. In particular, it sheds
serious doubts on an earlier interpretation implying the presence of a white
dwarf companion orbiting the star at an angular distance of $\sim$0.4 arcsec
from its centre and currently west of it.
