  It has been asserted that the primary star in the HD 189733 system steadily
accretes evaporated exospheric gases from its ``hot Jupiter'' companion, rather
like a T Tauri star accreting from a disk. We conduct statistical and
periodogram analyses of the photometric time series of the primary, as acquired
by the automated photoelectric telescope (APT), Microvariability and
Oscillations of Stars (MOST), and Wise Observatory, to investigate this claim
with the goal of revealing the presence of accretion shocks or photospheric
accretion hotspots as are found in T Tauri systems such as AA Tau. None of the
anticipated features were found. We re-analyze existing radio, optical,
ultraviolet, and X-ray data within the framework of accreting T Tauri systems
to determine physical quantities such as plasma density and temperature,
accretion rate, and flare lengths. We find that with an accretion rate of
$\dot{M}\sim10^{9}$ to 10$^{11}$ g s$^{-1}$, the star is more similar to a
system that intermittently absorbs gas from sungrazing comets in outburst than
classical T Tauri systems, which have accretion rates at least two orders of
magnitude larger. If such accretion exists, it would result in undetectably low
activity at all wavelengths. Alternatively, all of the emission properties
observed thus far are in agreement with stellar activity from a magnetically
active star.
