Accretion Discs Trapped Near Corotation

TL;DR

This paper investigates how accretion discs around magnetized, rotating stars can become 'trapped' near the corotation radius, exhibiting steady or cyclic accretion, with implications for stellar spin evolution and observed variability.

Contribution

It introduces the concept of trapped disc states near corotation, exploring their stability, evolution, and impact on star spin, supported by long-term simulations and analysis.

Findings

Discs can remain near corotation even at low accretion rates.

Two instability regions identified: outside mass buildup and near the transition zone.

Cyclic accretion influences stellar spin evolution and matches observed variability in young stars.

Abstract

We show that discs accreting onto the magnetosphere of a rotating star can end up in a 'trapped' state, in which the inner edge of the disc stays near the corotation radius, even at low and varying accretion rates. The accretion in these trapped states can be steady or cyclic; we explore these states over wide range of parameter space. We find two distinct regions of instability, one related to the buildup and release of mass in the disk outside corotation, the other to mass storage within the transition region near corotation. With a set of calculations over long time scales we show how trapped states evolve from both nonaccreting and fully accreting initial conditions, and also calculate the effects of cyclic accretion on the spin evolution of the star. Observations of cycles such as found here would provide important clues on the physics of magnetospheric accretion. Recent observations of cyclic and other unusual variability in T Tauri stars (EXors) and X-ray binaries are discussed in this context.