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The exoplanet WASP-12b is the prototype for the emerging class of ultra-hot,Jupiter-mass exoplanets. Past models have predicted---and near ultra-violetobservations have shown---that this planet is losing mass. We present ananalysis of two sets of 3.6 $\mu$m and 4.5 $\mu$m $\textit{Spitzer}$ phasecurve observations of the system which show clear evidence of infraredradiation from gas stripped from the planet, and the gas appears to be flowingdirectly toward or away from the host star. This accretion signature is onlyseen at 4.5 $\mu$m, not at 3.6 $\mu$m, which is indicative either of COemission at the longer wavelength or blackbody emission from cool, $\lesssim$600 K gas. It is unclear why WASP-12b is the only ultra-hot Jupiter to exhibitthis mass loss signature, but perhaps WASP-12b's orbit is decaying as some haveclaimed, while the orbits of other exoplanets may be more stable;alternatively, the high energy irradiation from WASP-12A may be stronger thanthe other host stars. We also find evidence for phase offset variability at thelevel of $6.4\sigma$ ($46.2^{\circ}$) at 3.6 $\mu$m.

Mass Loss from the Exoplanet WASP-12b Inferred from $\textit{Spitzer}$ Phase Curves