  We study the kinematics of the recently discovered Corona Australis (CrA)
chain of clusters by examining the 3D space motion of its young stars using
Gaia DR3 and APOGEE-2 data. While we observe linear expansion between the
clusters in the Cartesian XY directions, the expansion along Z exhibits a
curved pattern. To our knowledge, this is the first time such a nonlinear
velocity-position relation has been observed for stellar clusters. We propose a
scenario to explain our findings, in which the observed gradient is caused by
stellar feedback, accelerating the gas away from the Galactic plane. A
traceback analysis confirms that the CrA star formation complex was located
near the central clusters of the Scorpius Centaurus (Sco-Cen) OB association
10-15 Myr ago. It contains massive stars and thus offers a natural source of
feedback. Based on the velocity of the youngest unbound CrA cluster, we
estimate that a median number of about two supernovae would have been
sufficient to inject the present-day kinetic energy of the CrA molecular cloud.
This number agrees with that of recent studies. The head-tail morphology of the
CrA molecular cloud further supports the proposed feedback scenario, in which a
feedback force pushed the primordial cloud from the Galactic north, leading to
the current separation of 100 pc from the center of Sco-Cen. The formation of
spatially and temporally well-defined star formation patterns, such as the CrA
chain of clusters, is likely a common process in massive star-forming regions.
