Observational limits on the spin-down torque of Accretion Powered Stellar Winds

TL;DR

This study investigates whether accretion-powered stellar winds can explain the slow rotation of classical T Tauri stars by analyzing observational data and theoretical models, concluding that such winds are unlikely to be the sole spin-down mechanism.

Contribution

The paper provides observational constraints on the efficiency of accretion-powered stellar winds in spinning down young stars, challenging previous models that suggested they could be the main mechanism.

Findings

Luminous stars with high UV luminosity do not support spin equilibrium via stellar winds.

Lower luminosity stars could be compatible with zero torque, but require demanding wind conditions.

Accretion-powered stellar winds are unlikely to fully explain the observed slow rotation of CTTS.

Abstract

The rotation period of classical T Tauri stars (CTTS) represents a longstanding puzzle. While young low-mass stars show a wide range of rotation periods, many CTTS are slow rotators, spinning at a small fraction of break-up, and their rotation period does not seem to shorten, despite the fact that they are actively accreting and contracting. Matt & Pudritz (2005) proposed that the spin-down torque of a stellar wind powered by a fraction of the accretion energy would be strong enough to balance the spin-up torque due to accretion. Since this model establishes a direct relation between accretion and ejection, the observable stellar parameters (mass, radius, rotation period, magnetic field) and the accretion diagnostics (accretion shock luminosity), can be used to constraint the wind characteristics. In particular, since the accretion energy powers both the stellar wind and the shock emission, we show in this letter how the accretion shock luminosity L_UV can provide upper limits to the spin-down efficiency of the stellar wind. It is found that luminous sources with L_UV > 0.1 L_Sun and typical dipolar field components < 1 kG do not allow spin equilibrium solutions. Lower luminosity stars (L_UV < 0.1 L_Sun) are compatible with a zero-torque condition, but the corresponding stellar winds are still very demanding in terms of mass and energy flux. We therefore conclude that accretion powered stellar winds are unlikely to be the sole mechanism to provide an efficient spin-down torque for accreting classical T Tauri stars.