Turbulent Disk Simulations

About

A suite of AGAMA / Ramses N-body/hydrodynamical simulations of isolated, gas-rich, star-forming galaxies, aimed at understanding the properties of primeval galaxies in the early Universe. The high gas surface densities encourage vigorous star formation, which in turn couples with the gas to drive turbulence self-consistently. We explore three distinct histories: (i) there is no ongoing accretion and the gas is used up by the star formation; (ii) the star-forming gas is replenished by cooling in the hot halo gas; (iii) we revisit these models in the presence of a strong perturbing force (COMING SOON IN 2024).

Team

Model overview

Table 1. Base models. The DM halo in isolation follows roughly an NFW profile with a mass of \(10^{11} ~{\rm M_\odot}\), a virial radius of 36.96 kpc and a scaleradius of 9.13 kpc
Name	Alias	Disk Mass	Disk Scalength	\( f_{\rm disk} \)\(^a\)	\( f_{\rm gas}\)\(^b\)	Metallcity\(^c\)	Completed	Animation\(^d\)
		(\(10^{8} ~{\rm M_\odot}\))	(kpc)			(Z\(_\odot\))	(to \(\sim\)2 Gyr)	On-the-fly	Post-processed

Notes. \(^a\) Initial disk mass fraction. \(^b\) Initial gas fraction. \(^c\) Initial gas metallicity. \(^d\) The hyperlink attached to the checkmark leads to the corresponding animation. \(^e\) First introduced in Bland-Hawthorn et al. (2023).

Table 2. Model variations, consisting of a base model and an additional feature, or a variation thereof
Name	Alias	Base model	Additional Feature	Completed	Animation\(^a\)
				(to \(\sim\)2 Gyr)	On-the-fly	Post-processed

Notes. \(^a\) The hyperlink attached to the checkmark leads to the corresponding animation.

Animations (on-the-fly)

The following animations have been created on-the-fly. They differ from the post-processed animations in that they have a higher time resolution (\(\sim\)1 Myr rather than \(\sim\)10 Myr), but they show only the evolution of the new-born stars, the gas density and the gas temperature on a face-on projection.

Base models

Extended models

Animations (post-processed)

The following animations have been created in post-processing. They differ from the on-the-fly animations in that they have a lower time resolution (\(\sim\)10 Myr rather than \(\sim\)1 Myr), and that they show the evolution of the surface density of all disk components (pre-existing stars, and - if available - new-born stars, gas) along three orthogonal projections.