Characterising thermal sweeping: a rapid disc dispersal mechanism

TL;DR

This study investigates the rapid disc dispersal mechanism called thermal sweeping in protoplanetary discs, using radiation-hydrodynamic simulations to identify the critical conditions leading to swift destruction.

Contribution

The paper develops an analytic model for thermal sweeping, linking critical surface density to X-ray luminosity, stellar mass, and inner hole radius, advancing understanding of disc dispersal processes.

Findings

Critical surface density scales linearly with X-ray luminosity.

Thermal sweeping occurs when inner holes reach 20-40 AU.

Transition discs with large holes and no accretion are unlikely to undergo thermal sweeping.

Abstract

(Abridged) We consider the properties of protoplanetary discs that are undergoing inside-out clearing by photoevaporation. In particular, we aim to characterise the conditions under which a protoplanetary disc may undergo `thermal sweeping', a rapid (< 1e4 years) disc destruction mechanism proposed to occur when a clearing disc reaches sufficiently low surface density at its inner edge and where the disc is unstable to runaway penetration by the X-rays. We use a large suite of 1D radiation-hydrodynamic simulations to probe the observable parameter space, which is unfeasible in higher dimensions. These models allow us to determine the surface density at which thermal sweeping will take over the disc's evolution and to evaluate this critical surface density as a function of X-ray luminosity, stellar mass and inner hole radius. We find that this critical surface density scales linearly with X-ray luminosity, increases with inner hole radius and decreases with stellar mass and we develop an analytic model that reproduces these results. This surface density criterion is then used to determine the evolutionary state of protoplanetary discs at the point that they become unstable to destruction by thermal sweeping. We find that transition discs created by photoevaporation will undergo thermal sweeping when their inner holes reach 20-40 AU, implying that transition discs with large holes and no accretion (which were previously a predicted outcome of the later stages of all flavours of photoevaporation model) will not form. We emphasise that the surface density criteria that we have developed apply to all situations where the disc develops an inner hole that is optically thin to X-rays. It thus applies not only to the case of holes originally created by photoevaporation but also to holes formed, for example, by the tidal influence of planets.