The life cycle of starbursting circumnuclear gas discs

TL;DR

This paper uses high-resolution hydrodynamical simulations to explore the evolution of circumnuclear gas discs in galaxies, revealing how gravitational instabilities lead to starburst activity and influence galactic nucleus life cycles.

Contribution

It presents a self-consistent simulation framework that models star formation, stellar feedback, and gas dynamics in circumnuclear discs, aligning with recent observations of galactic nuclei.

Findings

Simulations reproduce observed gas and stellar masses in galactic nuclei.

Gravitational instabilities cause clump formation and starbursts.

Feedback processes influence gas dispersal and disc evolution.

Abstract

High-resolution observations from the sub-mm to the optical wavelength regime resolve the central few 100pc region of nearby galaxies in great detail. They reveal a large diversity of features: thick gas and stellar discs, nuclear starbursts, in- and outflows, central activity, jet interaction, etc. Concentrating on the role circumnuclear discs play in the life cycles of galactic nuclei, we employ 3D adaptive mesh refinement hydrodynamical simulations with the RAMSES code to self-consistently trace the evolution from a quasi-stable gas disc, undergoing gravitational (Toomre) instability, the formation of clumps and stars and the disc's subsequent, partial dispersal via stellar feedback. Our approach builds upon the observational finding that many nearby Seyfert galaxies have undergone intense nuclear starbursts in their recent past and in many nearby sources star formation is concentrated in a handful of clumps on a few 100pc distant from the galactic centre. We show that such observations can be understood as the result of gravitational instabilities in dense circumnuclear discs. By comparing these simulations to available integral field unit observations of a sample of nearby galactic nuclei, we find consistent gas and stellar masses, kinematics, star formation and outflow properties. Important ingredients in the simulations are the self-consistent treatment of star formation and the dynamical evolution of the stellar distribution as well as the modelling of a delay time distribution for the supernova feedback. The knowledge of the resulting simulated density structure and kinematics on pc scale is vital for understanding inflow and feedback processes towards galactic scales.