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We present H-band polarized scattered light imagery and JHK high-contrastspectroscopy of the protoplanetary disk around HD 163296 observed with theHiCIAO and SCExAO/CHARIS instruments at Subaru Observatory. The polarimetricimagery resolve a broken ring structure surrounding HD 163296 that peaks at adistance along the major axis of 0.65 (66 AU) and extends out to 0.98 (100 AU)along the major axis. Our 2011 H-band data exhibit clear axisymmetry, with theNW- and SE- side of the disk exhibiting similar intensities. Our data areclearly different than 2016 epoch H-band observations from VLT/SPHERE thatfound a strong 2.7x asymmetry between the NW- and SE-side of the disk.Collectively, these results indicate the presence of time variable,non-azimuthally symmetric illumination of the outer disk. Based on our 3D-MCRTmodeling of contemporaneous IR spectroscopic and H-band polarized intensityimagery of the system, we suggest that while the system could plausibly host aninclined inner disk component, such a component is unlikely to be responsiblefor producing the observed time-dependent azimuthal variations in the outerscattered light disk of the system. While our SCExAO/CHARIS data are sensitiveenough to recover the planet candidate identified from NIRC2 in the thermal IR,we fail to detect an object with a corresponding JHK brightness estimated fromthe atmospheric models of Baraffe et al. 2003. This suggests that the candidateis either fainter in JHK bands than model predictions, possibly due toextinction from the disk or atmospheric dust/clouds, or that it is an artifactof the dataset/data processing. Our SCExAO/CHARIS data lower the IR mass limitsfor planets inferred at larger stellocentric separations; however, theseALMA-predicted protoplanet candidates are currently still consistent withdirect imaging constraints.

Multi-epoch Direct Imaging and Time-Variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk