Work

Effect of irradiation model on 2D hydrodynamic simulations of self-gravitating protoplanetary discs

Year: 2025

Type: article

Abstract: ABSTRACT Young protoplanetary discs are expected to be gravitationally unstable, which can drive angular momentum transport as well as be a potential mechanism for planet formation. Gravitational instability is most prevalent in the outer disc where cooling time-scales are short. At large radii, stellar irradiation makes a significant contribution to disc heating and is expected to suppress instability. In this study, we compare two models of implementing irradiation in 2D hydrodynamic simulations of self-gravitating discs: supplying a constant heating rate per unit mass and per unit area of the disc. In the former case, instability is quenched once the stellar irradiation becomes the dominant heating source. In the latter case, we find instability persists under high levels of irradiation, despite large values of the Toomre Q parameter, in agreement with analytic predictions. Fragmentation was able to occur in this regime with the critical cooling time-scale required decreasing as irradiation is increased, corresponding to a maximum threshold for the viscosity parameter: $\alpha \sim 0.03-0.09$.

Source: Monthly Notices of the Royal Astronomical Society

DOI: 10.1093/mnras/staf644

Authors: Caitriona S Leedham, Richard A Booth, Cathie J Clarke

Institutions: University of Cambridge, University of Leeds

Language: English

Topic: Astrophysics and Star Formation Studies

Subfield: Astronomy and Astrophysics

Field: Physics and Astronomy

Domain: Physical Sciences

Open Access status: gold

Estimated APC paid: $3,046