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- W2232770739 abstract "Observations of the youngest planets (∼1–10 Myr for a transitional disk) will increase the accuracy of our planet formation models. Unfortunately, observations of such planets are challenging and time-consuming to undertake, even in ideal circumstances. Therefore, we propose the determination of a set of markers that can preselect promising exoplanet-hosting candidate disks. To this end, N-body simulations were conducted to investigate the effect of an embedded Jupiter-mass planet on the dynamics of the surrounding planetesimal disk and the resulting creation of second-generation collisional dust. We use a new collision model that allows fragmentation and erosion of planetesimals, and dust-sized fragments are simulated in a post-process step including non-gravitational forces due to stellar radiation and a gaseous protoplanetary disk. Synthetic images from our numerical simulations show a bright double ring at 850 μm for a low-eccentricity planet, whereas a high-eccentricity planet would produce a characteristic inner ring with asymmetries in the disk. In the presence of first-generation primordial dust these markers would be difficult to detect far from the orbit of the embedded planet, but would be detectable inside a gap of planetary origin in a transitional disk." @default.
- W2232770739 created "2016-06-24" @default.
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- W2232770739 date "2016-03-15" @default.
- W2232770739 modified "2023-10-16" @default.
- W2232770739 title "HIDING IN THE SHADOWS. II. COLLISIONAL DUST AS EXOPLANET MARKERS" @default.
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- W2232770739 doi "https://doi.org/10.3847/0004-637x/820/1/29" @default.
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