Date:
Tue, 01/04/202512:30-13:30
Speaker: Omry Ginzburg (Racah Institute)
Title: Turbulence in high redshift massive disks - origin & implications
Abstract:Star formation (SF) is the main physical process that determines the evolution and fate of galaxies.Observationally, most SF occurs in rotation-dominated disk galaxies, which, at high redshifts, form by the accretion of high angular momentum, cold streams of gas originating from the cosmic web. Being the main hosts of SF, the processes that govern the formation and evolution of disk galaxies are an important research subject.Despite variations in mass, size, and gas fractions between disk galaxies, observations suggest that there are several features that are common between disks, two of them being the perturbed clumpy structure and supersonic turbulence.
In this talk, I will discuss how these two features are intimately related and govern the dynamical and structural evolution of a galaxy. I will present a simple theoretical toy model for how turbulence is sustained in disks over several epochs. Also, I will show results from numerical simulations on how a compressible turbulence can enhance clump formation in galactic disks. Finally, I will show how deep learning can be used to study the longevity of these clumps observationally, by training neural networks on simulated clumps from cosmological simulations.
https://huji.zoom.us/j/84347178812?pwd=O5pq5eIDVgQe2PYjb1wWDAeChFbM3r.1
Meeting ID: 843 4717 8812
Passcode: 575367
Contact: Zhiyuan Yao
Title: Turbulence in high redshift massive disks - origin & implications
Abstract:Star formation (SF) is the main physical process that determines the evolution and fate of galaxies.Observationally, most SF occurs in rotation-dominated disk galaxies, which, at high redshifts, form by the accretion of high angular momentum, cold streams of gas originating from the cosmic web. Being the main hosts of SF, the processes that govern the formation and evolution of disk galaxies are an important research subject.Despite variations in mass, size, and gas fractions between disk galaxies, observations suggest that there are several features that are common between disks, two of them being the perturbed clumpy structure and supersonic turbulence.
In this talk, I will discuss how these two features are intimately related and govern the dynamical and structural evolution of a galaxy. I will present a simple theoretical toy model for how turbulence is sustained in disks over several epochs. Also, I will show results from numerical simulations on how a compressible turbulence can enhance clump formation in galactic disks. Finally, I will show how deep learning can be used to study the longevity of these clumps observationally, by training neural networks on simulated clumps from cosmological simulations.
https://huji.zoom.us/j/84347178812?pwd=O5pq5eIDVgQe2PYjb1wWDAeChFbM3r.1
Meeting ID: 843 4717 8812
Passcode: 575367
Contact: Zhiyuan Yao