2-D simulations of FU Orionis disk outbursts

TL;DR

This paper presents advanced 2D models of FU Orionis disk outbursts, highlighting the roles of gravitational and magnetorotational instabilities, and emphasizes the importance of vertical disk structure and convection in outburst dynamics.

Contribution

It introduces a comprehensive 2D, axisymmetric model with full vertical structure and a new radiative boundary condition, advancing understanding of FU Ori outburst mechanisms.

Findings

Outbursts driven by gravitational instability leading to magnetorotational instability.

Vertical structure and convection are crucial for accurate outburst modeling.

Models align with observed spectra, accretion rates, and decay timescales.

Abstract

We have developed time-dependent models of FU Ori accretion outbursts to explore the physical properties of protostellar disks. Our two-dimensional, axisymmetric models incorporate full vertical structure with a new treatment of the radiative boundary condition for the disk photosphere. We find that FU Ori-type outbursts can be explained by a slow accumulation of matter due to gravitational instability. Eventually this triggers the magnetorotational instability, which leads to rapid accretion. The thermal instability is triggered in the inner disk but this instability is not necessary for the outburst. An accurate disk vertical structure, including convection, is important for understanding the outburst behavior. Large convective eddies develop during the high state in the inner disk. The models are in agreement with Spitzer IRS spectra and also with peak accretion rates and decay timescales of observed outbursts, though some objects show faster rise timescale. We also propose that convection may account for the observed mild-supersonic turbulence and the short-timescale variations of FU Orionis objects.