Spin equilibrium in strongly-magnetized accreting stars
arXiv:1609.08654 · doi:10.1093/mnras/stx1306
Abstract
Strongly magnetized accreting stars are often hypothesized to be in `spin equilibrium' with their surrounding accretion flows, which requires that the accretion rate changes more slowly than it takes the star to reach spin equilibrium. This is not true for most magnetically accreting stars, which have strongly variable accretion outbursts on time-scales much shorter than the time it would take to reach spin equilibrium. This paper examines how accretion outbursts affect the time a star takes to reach spin equilibrium and its final equilibrium spin period. I consider several different models for angular momentum loss -- either carried away in an outflow, lost to a stellar wind, or transferred back to the accretion disc (the `trapped disc'). For transient sources, the outflow scenario leads to significantly longer times to reach spin equilibrium (10x), and shorter equilibrium spin periods than would be expected from spin equilibrium arguments, while the `trapped disc' does not. The results suggest that disc trapping plays a significant role in the spin evolution of strongly magnetic stars, with some caveats for young stellar objects.
version accepted by MNRAS; some significant changes to conclusions about FU Ori stars
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