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
- Joss Bland-Hawthorn (U Sydney)
- Thor Tepper-García (U Sydney)
- Oscar Agertz (U Lund)
- Christoph Federrath (ANU)
Model overview
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).
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.