Author(s): E.A. Rich, J. Wisniewski, Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, Oklahoma, UNITED STATES|T. Currie, Ames Research Center, Mountain View, California, UNITED STATES|M. Sitko, University of Cincinnati , Cincinnati, Ohio, UNITED STATES|C. Grady, Goddard Space Flight Center, Greenbelt, Maryland, UNITED STATES|C. Grady, Eureka Scientific, Oakland, California, UNITED STATES|M. Fukagawa, Osaka University, Toyonaka, Osaka, JAPAN|
Institution(s): 1. Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK, United States. 2. Ames Research Center, Mountain View, CA, United States. 3. University of Cincinnati , Cincinnati, OH, United States. 4. Goddard Space Flight Center, Greenbelt, MD, United States. 5. Eureka Scientific, Oakland, CA, United States. 6. Osaka University, Toyonaka, Osaka, Japan.
Contributing team(s): SEEDS Team
We present multi-epoch observations of the protoplanetary disk around HD 163296 with Subaru/HiCIAO and Subaru/SCExAO along with contemporaneous infrared spectroscopic observations. We modeled our contemporaneous data with a Monte Carlo Radiative Transfer code and show that the Subaru/HiCIAO image and SED of HD 163296 are consistent with a thin disk and an optically thin envelope around the star. Our observations join a host of other images of HD 163296 taken from 2011 to 2018, which collectively exhibit clear evidence of variability in the spatially resolved scattered light disk surrounding the star. We suggest that the observed asymmetrical change in flux is caused by shadowing either from dust ejected above the plane of the disk or local warping of the disk. Finally, our SCExAO data do not confirm the purported detection of a candidate planetary mass object located at 67 au from the central star that was reported by Guidi+ (2018) based on analysis of Keck L' observations. This research was supported by grant NNX17AF88G from NASA's Exoplanet Research Program and from HST GO-15437.