Abstract Rayleigh–Taylor (RT) and Richtmyer–Meshkov (RM) instabilities are well-known
pathways towards turbulent mixing layers, in many cases characterized by significant mass …

The theory of the Rayleigh-Taylor instability of accelerated fluid layers is systematically
developed from basic fluid equations. Starting with the classical potential flow theory for …

We present results of 3D simulations of magnetohydrodynamics (MHD) instabilities at the
accretion disc–magnetosphere boundary. The instability is Rayleigh–Taylor, and develops …

We report on the first global three-dimensional (3D) MHD simulations of disk accretion onto
a rotating magnetized star through the Rayleigh-Taylor instability. The star has a dipole field …

We present three-dimensional magnetohydrodynamic (MHD) simulations of radiatively
inefficient accretion flow around black holes. General relativistic effects are simulated by …

We study the magnetic Rayleigh-Taylor instability in three dimensions, with focus on the
nonlinear structure and evolution that results from different initial field configurations. We …

We study the magnetic Rayleigh-Taylor instability in relativistic collisionless plasma, as an
astrophysical process for nonthermal particle acceleration. We consider dense plasma on …

Motivated by considerations of the solar toroidal magnetic field we have studied the
behaviour of a layer of uniform magnetic field embedded in a convectively stable …

We present a numerical investigation of the development of Rayleigh-Taylor instability at the
interface between an expanding Pulsar Wind Nebula and its surrounding Supernova …

In accretion discs with large-scale ordered magnetic fields, the magnetorotational instability
(MRI) is marginally suppressed, so other processes may drive angular momentum transport …