  Observations of the high-mass gamma-ray binary LS 2883/PSR B1259--63 with the
Chandra X-ray Observatory during the 2011--2014 and 2014--2017 binary cycles
have shown X-ray emitting clumps, presumably ejected from the binary during
periastron passages. These clumps traveled at projected velocities of $\sim0.1
c$ and have shown evidence of being accelerated. The clumps also evolved in
shape, size, and flux. We monitored this binary with Chandra during the
2017--2021 binary cycle to search for additional X-ray emitting ejections.
While we find evidence of extended emission in two of the six observations, it
is unlike the clumps observed in the previous three binary cycles. More
specifically, the extended emission is not well localized and no bright clump
is observed moving away from the binary. It is still unclear what caused the
lack of X-ray emitting clump in this orbital cycle, but it may be due to
changes in the decretion disk of the Be star.
