Discs are born eccentric

TL;DR

This paper predicts that early star formation discs are inherently eccentric based on non-ideal MHD simulations, challenging current models of disc evolution and suggesting new circularization mechanisms.

Contribution

It provides the first detailed simulation-based prediction that young star formation discs are naturally eccentric, with implications for planet formation theories.

Findings

Discs formed in simulations have eccentricities around 0.1.

Eccentricity persists despite symmetric initial conditions.

Results challenge existing models of disc circularization.

Abstract

Recent observations have begun probing the early phases of disc formation, but little data yet exists on disc structure and morphology of Class 0 objects. Using simulations, we are able to lay out predictions of disc morphologies expected in future surveys of young discs. Based on detailed simulations of ab initio star formation by core collapse, we predict that early discs must be eccentric. In this letter, we study the morphology and, in particular, the eccentricity of discs formed in non-ideal magnetohydrodynamic (MHD) collapse simulations. We attempt to show that discs formed by cloud collapse are likely to be eccentric. We ran non-ideal MHD collapse simulations in the adaptive mesh refinement code RAMSES with radiative transfer. We used state-of-the-art analysis methods to measure the disc eccentricity. We find that despite no asymmetry in the initial conditions, the discs formed are eccentric, with eccentricities on the order of 0.1. These results may have important implications for protoplanetary disc dynamics and planet formation. The presence of eccentricity in young discs that is not seen at later stages of disc evolution is in tension with current viscous eccentricity damping models. This implies that there may be an as-yet undiscovered circularisation mechanism in circumstellar discs.