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Abstract

The disk around the closest Herbig Ae star, HD169142, has been studied extensively at multiple wavelengths. At an almost face-on inclination, it reveals three major components: a yet unresolved ring/halo at only 0.1 au from the star, a bright ring around 20 au, and an outer disk stretching from 55-122 au. The gaps are emptied from dust and gas, which is a strong indicator for the presence of planets. In our series of observations (2012-2018) we report for the first time the presence of brightness variations inside the major ring at 20 au (Bertrang+2018, Bertrang in prep.). Assuming Keplerian velocity, we determine that the brightness dip is consistent with a shadow cast by a Jupiter-mass planet or brown dwarf surrounded by dust at a radial distance of only 12au, an orbit comparable to Jupiter's. For this talk I will reveal new multi- wavelength observations together with radiative transfer models and hydrodynamical simulations which support the picture that HD169142 might be a young version of a multi-planet system such as HR8799 or our own solar system.