Speaker
Description
Radiative turbulent mixing layers are central to the evolution of interstellar and circumgalactic gas, characterized by rapid radiative cooling at intermediate temperatures. While recent studies have focused extensively on cooling driven by the Kelvin-Helmholtz (KH) instability, the role of the Rayleigh-Taylor (RT) instability, a key mechanism in supernova remnants, remains largely underexplored.
Using the 3D hydrodynamical code GIZMO, we investigate cooling within RT-driven mixing layers and find that the cooling rate is governed by the ratio of the mixing time to the cooling time, which follows a scaling relation similar to KH-driven mixing layers, suggesting a common turbulent nature despite very different driving mechanisms.
Furthermore, by directly resolving the Field length, we examine the impact of thermal conduction on global cooling rates and establish rigorous resolution requirements for accurate modeling.
| Participate the oral/poster presentation award competition | Yes |
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