University of Cambridge > > Exoplanet Seminars > Co-evolution of (Proto)Planets and Substructures in Disks

Co-evolution of (Proto)Planets and Substructures in Disks

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If you have a question about this talk, please contact Dr Emily Sandford.

Protoplanetary disks, the birthplace of planets, exhibit prominent features such as bright rings and dark gaps in both continuum and line-emission maps. In my presentation, I will introduce two perspectives that establish connections between protoplanets, disk substructures, and astrochemistry.

In the context of continuum emission, the accumulation of pebbles within these rings plays a crucial role in facilitating planetesimal formation and subsequent planet assembly. Using N-body simulations, we investigate the feasibility of planet formation within pebble rings and explore how this mechanism can explain the presence of mature planetary systems observed within debris disks, like the ones in HR 8799 .

Furthermore, the presence of rings in molecular emissions also offers insights into the potential circumstance of planet formation. By employing multi-fluid hydrodynamical simulations that consider evaporation fronts, we simulate the process of an accreting planet locally heating its surroundings, creating a gap in the disk, and initiating Carbon photochemistry. The simulation output provides a plausible explanation for certain molecular line distributions observed by ALMA .

This talk is part of the Exoplanet Seminars series.

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