Currently, we are simulating moist convection with Earth-like parameters, including rotation, to better understand atmospheric dynamics. These high-resolution simulations aim to capture the complex interplay of turbulence, convection, and large-scale circulation.
We perform direct numerical simulations of supersonic turbulence using GPU-accelerated DHARA and high-order TENO scheme. Our focus is on multiscale energy transfers, shock–turbulence interactions, and their role in astrophysical and high-speed flow environments.
We investigates compressible turbulent convection at extreme Rayleigh numbers. These studies reveal classical heat-transport scaling laws and provide insights into highly nonlinear regimes relevant to both astrophysics and geophysical flows.
We coarse-grain the Navier–Stokes equations shell by shell in Fourier space. Using a first-order Green’s function, we obtain a scale-dependent renormalized viscosity, which converges across shells to give the effective inertial-range transport.
We study the structure and key processes in neutron stars, focusing on magnetic field dynamics such as Ohmic dissipation and Hall drift. The formalism of electron magnetohydrodynamics (EMHD) is applied to model the crust.
We study the dynamics and trapping of acoustic oscillations in thin accretion disks, focusing on their behavior near rotating black holes and related astrophysical effects.