Loren E. Held
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View article: Magnetorotational instability-driven <i>α</i>Ω dynamo at high Prandtl numbers
Magnetorotational instability-driven <i>α</i>Ω dynamo at high Prandtl numbers Open
Context. To power gamma-ray bursts and other high-energy events, large-scale magnetic fields are required to extract rotational energy from compact objects such as black holes and neutron stars. Magnetorotational instability (MRI) is a key…
View article: MRI-driven $αΩ$ dynamo at high Pm numbers
MRI-driven $αΩ$ dynamo at high Pm numbers Open
To power gamma-ray bursts and other high-energy events, large-scale magnetic fields are required to extract rotational energy from compact objects such as black holes and neutron stars. The magnetorotational instability (MRI) is a key mech…
View article: Instability and warping in vertically oscillating accretion discs
Instability and warping in vertically oscillating accretion discs Open
Many accretion discs have been found to be distorted: either warped due to a misalignment in the system, or non-circular as a result of orbital eccentricity or tidal deformation by a binary companion. Warped, eccentric, and tidally distort…
View article: Instability and warping in vertically oscillating accretion discs
Instability and warping in vertically oscillating accretion discs Open
Many accretion discs have been found to be distorted: either warped due a misalignment in the system, or non-circular as a result of orbital eccentricity or tidal deformation by a binary companion. Warped, eccentric, and tidally distorted …
View article: MRI turbulence in vertically stratified accretion discs at large magnetic Prandtl numbers
MRI turbulence in vertically stratified accretion discs at large magnetic Prandtl numbers Open
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 determined by the grid) and/or axisymmetric (invoking a…
View article: MRI turbulence in vertically stratified accretion discs at large magnetic Prandtl numbers
MRI turbulence in vertically stratified accretion discs at large magnetic Prandtl numbers Open
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 determined by the grid) and/or axisymmetric (invoking a…
View article: Implementation of advanced Riemann solvers in a neutrino-radiation magnetohydrodynamics code in numerical relativity and its application to a binary neutron star merger
Implementation of advanced Riemann solvers in a neutrino-radiation magnetohydrodynamics code in numerical relativity and its application to a binary neutron star merger Open
We implement advanced Riemann solvers HLLC and HLLD \cite{Mignone:2005ft,MUB:2009} together with an advanced constrained transport scheme \cite{Gardiner:2007nc} in a numerical-relativity neutrino-radiation magnetohydrodynamics code. We val…
View article: MRI turbulence in accretion discs at large magnetic Prandtl numbers
MRI turbulence in accretion discs at large magnetic Prandtl numbers Open
The effect of large magnetic Prandtl number $\text{Pm}$ (the ratio of viscosity to resistivity) on the turbulent transport and energetics of the magnetorotational instability (MRI) is poorly understood, despite the realization of this regi…
View article: Implementation of advanced Riemann solvers in a neutrino-radiation magnetohydrodynamics code in numerical relativity and its application to a binary neutron star merger
Implementation of advanced Riemann solvers in a neutrino-radiation magnetohydrodynamics code in numerical relativity and its application to a binary neutron star merger Open
We implement advanced Riemann solvers HLLC and HLLD \cite{Mignone:2005ft,MUB:2009} together with an advanced constrained transport scheme \cite{Gardiner:2007nc} in a numerical-relativity neutrino-radiation magnetohydrodynamics code. We val…
View article: The stress–pressure lag in MRI turbulence and its implications for thermal instability in accretion discs
The stress–pressure lag in MRI turbulence and its implications for thermal instability in accretion discs Open
The classical alpha-disc model assumes that the turbulent stress scales linearly with – and responds instantaneously to – the pressure. It is likely, however, that the stress possesses a non-negligible relaxation time and will lag behind t…
View article: Magnetohydrodynamic convection in accretion discs
Magnetohydrodynamic convection in accretion discs Open
Convection has been discussed in the field of accretion discs for several decades, both as a means of angular momentum transport and also because of its role in controlling discs’ vertical structure via heat transport. If the gas is suffic…
View article: Hydrodynamic and Magnetohydrodynamic Convection in Accretion Disks
Hydrodynamic and Magnetohydrodynamic Convection in Accretion Disks Open
The prevalence and consequences of convection perpendicular to the plane of accretion disks have been discussed for several decades. Recent simulations combining convection and the magnetorotational instability have given fresh impetus to …
View article: Hydrodynamic convection in accretion discs
Hydrodynamic convection in accretion discs Open
The prevalence and consequences of convection perpendicular to the plane of accretion discs have been discussed for several decades. Recent simulations combining convection and the magnetorotational instability have given fresh impetus to …