  Several "hot Jupiter" host stars appear to exhibit enhanced chromospheric
activity, coronal flaring, and starspot development synchronized to their
planetary orbits. These effects have been attributed to tidal and/or magnetic
interactions between the star and exoplanet. The best studied among such
systems is HD 189733, which has previously been observed from radio to X-ray
wavelengths. Here, I present ~4.75 GHz Arecibo radio telescope observations of
HD 189733 during a fraction of the exoplanet orbital phase range previously
associated with enhanced coronal X-ray flaring. No radio flares from the lower
corona were detected. I also leverage Microvariability and Oscillations of
Stars, Automated Photoelectric Telescope, and Wise photometry to measure the
occurences of minima associated with enhanced starspot activity. The phasing of
these minima with the exoplanet orbit does not reveal any synchronized active
region behavior. Moreover, for the first time, I combine X-ray, ultraviolet,
photometric, Ca II H&K, H-alpha, and radio observations of HD 189733 to conduct
an extensive, holistic reexamination of stellar activity in this system.
Through the presentation of new data, and by merging physical and statistical
analytic approaches, I demonstrate that the previously asserted enhancements in
activity, allegedly synchronized to certain exoplanet orbital phases, are
likely the result of inadequately sampled intrinsic stellar activity from an
active star, rather than star-planet interactions.
