Accretion discs as regulators of stellar angular momentum evolution in the ONC and Taurus-Auriga

TL;DR

This study investigates how accretion discs influence the angular momentum evolution of pre-main sequence stars in the ONC and Taurus-Auriga, revealing rapid disc dispersal and efficient angular momentum removal mechanisms.

Contribution

It provides a revised analysis of stellar angular momentum evolution using updated stellar parameters and classifies stars by disc presence, highlighting the role of disc dispersal and outflows.

Findings

Disc dispersal occurs rapidly at various ages.

Angular momentum decreases significantly during the Class II phase.

Post-disc dispersal, angular momentum remains nearly constant.

Abstract

In light of recent substantial updates to spectral type estimations and newly established intrinsic colours, effective temperatures, and bolometric corrections for pre-main sequence (PMS) stars, we re-address the theory of accretion-disc regulated stellar angular momentum (AM) evolution. We report on the compilation of a consistent sample of fully convective stars within two of the most well-studied and youngest, nearby regions of star formation: the Orion Nebula Cluster (ONC) and Taurus-Auriga. We calculate the average specific stellar AM ($j_{\star}$) assuming solid body rotation, using surface rotation periods gathered from the literature and new estimates of stellar radii and ages. We use published Spitzer IRAC fluxes to classify our stars as Class II or Class III and compare their $j_{\star}$ evolution. Our results suggest that disc dispersal is a rapid process that occurs at a variety of ages. We find a consistent $j_{\star}$ reduction rate between the Class II and Class III PMS stars which we interpret as indicating a period of accretion disc-regulated AM evolution followed by near-constant AM evolution once the disc has dissipated. Furthermore, assuming our observed spread in stellar ages is real, we find the removal rate of $j_{\star}$ during the Class II phase is more rapid than expected by contraction at constant stellar rotation rate. A much more efficient process of AM removal must exist, most likely in the form of an accretion-driven stellar wind or other outflow from the star-disc interaction region or extended disc surface.