Protostellar disks formed from rigidly rotating cores

TL;DR

This study uses 3D simulations to explore how initial core rotation affects protostellar disc formation, stability, and fragmentation, revealing conditions that lead to single or multiple star systems.

Contribution

It introduces a new criterion predicting disc fragmentation based on core rotation, mass, and size, and applies it to observed cores to assess their stability.

Findings

Cores with low rotation form stable, warm, centrally concentrated discs.

Rapidly rotating cores produce larger, cooler discs prone to fragmentation.

Most observed cores are stable against fragmentation due to low angular speeds.

Abstract

Abridged: We use three-dimensional SPH simulations to investigate the collapse of low-mass prestellar cores and the formation and early evolution of protostellar discs. The initial conditions are slightly supercritical Bonnor-Ebert spheres in rigid rotation. The core mass and initial radius are held fixed at M_O=6.1 M_sun and R_O=17,000 AU, and the only parameter that we vary is the initial angular speed \Omega_O. Protostellar discs forming from cores with \Omega_O<1.35 10d-13 1/s have radii between 100 and 300 AU and are quite centrally concentrated; due to heating by gas infall onto the disc and accretion onto the central object, they are also quite warm, T>100 K, and therefore stable against gravitational fragmentation. In contrast, more rapidly rotating cores form discs which are less concentrated and cooler, and have radii between 400 and 1000 AU; as a consequence they are prone to gravitational fragmentation and the formation of multiple systems. We derive a criterion that predicts whether a rigidly rotating core having given M_O, R_O and \Omega_O will produce a protostellar disc which fragments whilst material is still infalling from the core envelope. We then apply this criterion to core samples for which M_O, R_O and \Omega_O have been estimated observationally. We conclude that the observed cores are stable against fragmentation at this stage, due to their low angular speeds and the heat delivered at the accretion shock where the infalling material hits the disc.