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It has been asserted that the primary star in the HD 189733 system steadilyaccretes evaporated exospheric gases from its ``hot Jupiter'' companion, ratherlike a T Tauri star accreting from a disk. We conduct statistical andperiodogram analyses of the photometric time series of the primary, as acquiredby the automated photoelectric telescope (APT), Microvariability andOscillations of Stars (MOST), and Wise Observatory, to investigate this claimwith the goal of revealing the presence of accretion shocks or photosphericaccretion hotspots as are found in T Tauri systems such as AA Tau. None of theanticipated features were found. We re-analyze existing radio, optical,ultraviolet, and X-ray data within the framework of accreting T Tauri systemsto 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 asystem that intermittently absorbs gas from sungrazing comets in outburst thanclassical T Tauri systems, which have accretion rates at least two orders ofmagnitude larger. If such accretion exists, it would result in undetectably lowactivity at all wavelengths. Alternatively, all of the emission propertiesobserved thus far are in agreement with stellar activity from a magneticallyactive star.

astrophysical journal/the astrophysical journal

ROME (Radio Observations of Magnetized Exoplanets). II. HD 189733 Does  Not Accrete Significant Material from its Exoplanet like a T Tauri Star from  A Disk