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Gravitational Instability in Irradiated Protoplanetary Discs

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Young protoplanetary discs are expected to be massive and self-gravitating. The resulting gravitational instability (GI) causes large spiral structures in the disc and is a potential formation mechanism of giant planets via direct collapse of overdense regions of gas. The onset of GI is sensitive to thermal processes in the disc. It is, therefore, influenced by irradiation, such as that from the central star, which is expected to suppress the instability. However, this is dependent on the exact implementation of heating. In this talk I will present the results of 2D hydrodynamic simulations comparing the outcomes of two different heating prescriptions and show that a disc heated per unit area remains gravitationally unstable even under high levels of irradiation.

This talk is part of the Institute of Astronomy Seminars series.

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