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Understanding the diversity of planets requires to study the morphology andthe physical conditions in the protoplanetary disks in which they form. Weobserved and spatially resolved the disk around the ~10 Myr old protoplanetarydisk HD 100453 in polarized scattered light with SPHERE/VLT at optical andnear-infrared wavelengths, reaching an angular resolution of ~0.02", and aninner working angle of ~0.09". We detect polarized scattered light up to ~0.42"(~48 au) and detect a cavity, a rim with azimuthal brightness variations at aninclination of 38 degrees, two shadows and two symmetric spiral arms. Thespiral arms originate near the location of the shadows, close to the semi majoraxis. We detect a faint spiral-like feature in the SW that can be interpretedas the scattering surface of the bottom side of the disk, if the disk istidally truncated by the M-dwarf companion currently seen at a projecteddistance of ~119 au. We construct a radiative transfer model that accounts forthe main characteristics of the features with an inner and outer diskmisaligned by ~72 degrees. The azimuthal brightness variations along the rimare well reproduced with the scattering phase function of the model. Whilespirals can be triggered by the tidal interaction with the companion, the closeproximity of the spirals to the shadows suggests that the shadows could alsoplay a role. The change in stellar illumination along the rim, induces anazimuthal variation of the scale height that can contribute to the brightnessvariations. Dark regions in polarized images of transition disks are nowdetected in a handful of disks and often interpreted as shadows due to amisaligned inner disk. The origin of such a misalignment in HD 100453, and ofthe spirals, is unclear, and might be due to a yet-undetected massive companioninside the cavity, and on an inclined orbit.

Shadows and spirals in the protoplanetary disk HD 100453