  The TESS spacecraft observed the asynchronous polar CD Ind at a two-minute
cadence almost continuously for 28 days in 2018, covering parts of 5
consecutive cycles of the system's 7.3-day beat period. These observations
provide the first uninterrupted photometry of a full spin-orbit beat cycle of
an asynchronous polar. Twice per beat cycle, the accretion flow switched
between magnetic poles on the white dwarf, causing the spin pulse of the white
dwarf (WD) to alternate between two waveforms after each pole-switch. An
analysis of the waveforms suggests that one accretion region is continuously
visible when it is active, while the other region experiences lengthy
self-eclipses by the white dwarf. We argue that the previously accepted periods
for both the binary orbit and the WD spin have been misidentified, and while
the cause of this misidentification is a subtle and easily overlooked effect,
it has profound consequences for the interpretation of the system's accretion
geometry and doubles the estimated time to resynchronization. Moreover, our
timings of the photometric maxima do not agree with the quadratic ephemeris
from Myers et al. (2017), and it is possible that the optical spin pulse might
be an unreliable indicator of the white dwarf's rotation. Finally, we use
Doppler tomography of archival time-resolved spectra from 2006 to study the
accretion flow. While the accretion flow showed a wider azimuthal extent than
is typical for synchronous polars, it was significantly less extended than in
the three other asynchronous polars for which Doppler tomography has been
reported.
