The magnetorotational instability (MRI) is an important process in sufficiently ionized
accretion discs, as it can create turbulence that acts as an effective viscosity, mediating …

Turbulence in three dimensions (3D) supports vortex stretching that has long been known to
accomplish energy transfer to small scales. Moreover, net energy transfer from large-scale …

The effect of large magnetic Prandtl number Pm (the ratio of viscosity to resistivity) on the
turbulent transport and energetics of the magnetorotational instability (MRI) is poorly …

We investigate sustenance and dependence on magnetic Prandtl number (Pm) for
magnetorotational instability (MRI)-driven turbulence in Keplerian disks with zero net …

We conduct a linear analysis of axisymmetric magnetorotational instability (MRI) in a
magnetized cylindrical Taylor-Couette (TC) flow for its standard version (SMRI) with a purely …

The discovery of the first binary neutron star merger, GW170817, has spawned a plethora of
global numerical relativity simulations. These simulations are often ideal (with dissipation …

Active Modes and Dynamical Balances in MRI Turbulence of Keplerian Disks with a Net
Vertical Magnetic Field - IOPscience This site uses cookies. By continuing to use this site you …

Observations, mainly of outbursts in dwarf novae, imply that the anomalous viscosity in
highly ionized accretion discs is magnetic in origin and requires that the plasma. We suggest …

Here, we address the turbulent dynamics of the gravitational instability in accretion disks,
retaining both radiative cooling and irradiation. Due to radiative cooling, the disk is unstable …

Origin of hydrodynamical instability and turbulence in the Keplerian accretion disc as well as
similar laboratory shear flows, eg plane Couette flow, is a long-standing puzzle. These flows …