Sean P. Matt

TL;DR: In this article, the angular momentum extracted by a wind from a pre-main-sequence star to the torques arising from the interaction between the star and its Keplerian accretion disk is compared.

TL;DR: In this article, a physically motivated scaling for the dependence of the stellar wind torque on the Rossby number was derived, which explains why the lowest mass stars are observed to maintain rapid rotation for much longer than solar-mass stars.

TL;DR: In this paper, the authors considered a dipolar stellar magnetic field, both quadrupolar and octupolar configurations, while also varying the rotation rate and the magnetic field strength, and gave a unique law that fits the data for every topology by formulating the torque in terms of the amount of open magnetic flux in the wind.

TL;DR: In this article, the authors used two-dimensional axisymmetric magnetohydrodynamic simulations to compute steady-state solutions for solar-like stellar winds from rotating stars with dipolar magnetic fields.

TL;DR: In this paper, the role of stellar winds in torquing down the stars was explored, and the stellar winds need to have relatively high outflow rates, and thus would likely be powered by the accretion process itself.