Detecting, modelling and characterising turbulent convection from the Sun to galaxy clusters
| When |
Sep 17, 2024
from 11:00 to 12:00 |
|---|---|
| Where | Salle des thèses |
| Contact Name | Julien Salort |
| Attendees |
François Rincon |
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Turbulent thermal convection is one of the main out-of-equilibrium fluid dynamics processes at work in astrophysical systems, and its study is of great importance to the broader understanding of turbulent heat, angular momentum, chemical, and magnetic-field transport, and dissipation in a variety of objects. Depending on plasma conditions, astrophysical convection can take a variety of forms, from standard, subsonic hydro and MHD convection driven by superadiabatic gradients in stars, to magnetized Braginskii-MHD-like buoyancy instabilities in the intracluster medium of galaxy clusters. In this talk, I will explore the theoretical, numerical, and observational challenges of, and recent progress in characterising astrophysical convection through two very different case studies: solar-surface convection, and the more speculative magneto-thermal instability in galaxy clusters. I will also explain how the high-temporal and spatial resolution imaging of convection at the surface of the Sun makes it an interesting and unique “fluid dynamics lab” to probe extreme regimes of turbulent (MHD) transport in astrophysics and beyond.