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Investigating the effect of radiation pressure on protoplanetary disc dispersal

Presentation #102.328 in the session Poster Session.

Published onJun 20, 2022
Investigating the effect of radiation pressure on protoplanetary disc dispersal

The current understanding of protoplanetary disc dispersal involves the removal of gas and dust via a photoevaporative wind generated by stellar heating of the disc. Previous models implied that there should be a large population of non-accreting discs with inner cavities due to the length of time needed to clear the outer disc. However, a lack of observations of such discs suggests that this clear-out must occur on shorter timescales. Work done by Owen & Kollmeier (2019) showed that these short timescales could be achieved by the removal of the dust component of the disc via radiation pressure from the central star. I am continuing this work by moving to a 2D framework that will incorporate a self-consistent calculation of the dust particle distribution in order to more accurately determine dust mass-loss rates. If the clear-out timescale remains short, this will support the conclusion that a combination of photoevaporation and radiation pressure mechanisms can lead to disc dispersal that fits the observational constraints.

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