  WR 20a is the most massive close-in binary known in our Galaxy. It is
composed of two $\approx$80 M$_\odot$ Wolf-Rayet stars with a short period of
$\approx$3.7 days in the open cluster Westerlund 2. As such, WR 20a presents us
with a unique laboratory for studying the currently uncertain physics of binary
evolution and compact object formation as well as for studying the wind
collision region in an massive eclipsing binary system. We use deep Chandra
observations of WR 20a to study the time variability of the wind collision
region between the two Wolf-Rayet stars and are able to produce an X-ray light
curve covering $\approx$2/3 of its orbital period. We find that the X-ray light
curve is asymmetric because the flux of one peak is 2.5$\sigma$ larger than the
flux of the other peak. This asymmetry could be caused by asymmetric mass-loss
from the two stars or by the lopsidedness of the wind collision region due to
the unusually fast rotation of the system. The X-ray light curve is also
shifted in phase space when compared to the optical light curves measured by
TESS and ASAS-SN. Additionally, we explore the ultimate fate of this system by
modeling the resultant binary black hole merger expected at the end of the two
stars' lives. We conclude that this system will evolve to be a representative
of the sub-population of LIGO progenitors of fast-spinning binary black hole
merger events.
