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Magnetic Prandtl number
The Role of MHD Turbulence in Magnetic Self-Excitation in The
Fluid Mechanics of Liquid Metal Batteries
Anomalous Viscosity, Resistivity, and Thermal Diffusivity of the Solar
Rayleigh-Bernard Convection Without Rotation and Magnetic Field
Toward a Self-Generating Magnetic Dynamo: the Role of Turbulence
Turbulent Magnetic Prandtl Number and Magnetic Diffusivity Quenching from Simulations
Arxiv:1904.00225V1 [Astro-Ph.SR] 30 Mar 2019 Bilities and Angular Momentum Transport
Turbulent Viscosity and Magnetic Prandtl Number from Simulations of Isotropically Forced Turbulence P
Experiments on Rayleigh–Bénard Convection, Magnetoconvection
A Multiscale Dynamo Model Driven by Quasi-Geostrophic Convection
How Magnetic Is the Solar Tachocline?
Small-Scale Dynamos in Simulations of Stratified Turbulent Convection
Arxiv:1109.4571V2 [Astro-Ph.CO] 20 Feb 2012 for Virtually All Astrophysical Objects
SASO-ISO-80000-11-2020-E.Pdf
Turbulent Geodynamo Simulations: a Leap Towards Earth's Core
Using Standard Syste
Beyond Ideal MHD
Dynamos and Differential Rotation: Advances at the Crossroads Of
Top View
Pl;Oe Flow Through a Solenoid of Finite Length
Mechanisms of Planetary and Stellar Dynamos
Abstracts Invited Speakers
Strong-Field Spherical Dynamos 3
Turbulent Viscosity and Magnetic Prandtl Number from Simulations of Isotropically Forced Turbulence P
Instabilities in Free-Surface Hartmann Flow at Low Magnetic Prandtl Numbers
Arxiv:1712.03787V1 [Physics.Flu-Dyn] 11 Dec 2017 Yia Flqi Easadslrsse Bet.A a As the Reaches Objects
Low Magnetic Prandtl Number Dynamos with Helical Forcing
MHD Turbulence at Moderate Magnetic Reynolds Number
Solar Magnetic Fields Over More Than five Decades in flux
Large-Wavelength Instabilities in Free-Surface Hartmann Flow at Low
Reversed Dynamo at Small Scales and Large Magnetic
UCLA Electronic Theses and Dissertations
Magnetohydrodynamic Flow and Heat Transfer Induced by a Shrinking Sheet
Experimental Investigation of Magnetohydrodynamic Flow for an Intense Proton Target
Intermittent Turbulent Dynamo at Very Low and High Magnetic Prandtl Numbers
Dependence on Magnetic Prandtl Number
Thermal Flux in Unsteady Rayleigh-B\'{E} Nard