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Related Concept Videos

Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

An electric field suffers a discontinuity at a surface charge. Similarly, a magnetic field is discontinuous at a surface current. The perpendicular component of a magnetic field is continuous across the interface of two magnetic mediums. In contrast, its parallel component, perpendicular to the current, is discontinuous by the amount equal to the product of the vacuum permeability and the surface current. Like the scalar potential in electrostatics, the vector potential is also continuous...
Magnetic Damping01:17

Magnetic Damping

Eddy currents can produce significant drag on motion, called magnetic damping. For instance, when a metallic pendulum bob swings between the poles of a strong magnet, significant drag acts on the bob as it enters and leaves the field, quickly damping the motion.
If, however, the bob is a slotted metal plate, the magnet produces a much smaller effect. When a slotted metal plate enters the field, an emf is induced by the change in flux; however, it is less effective because the slots limit the...
Energy In A Magnetic Field01:24

Energy In A Magnetic Field

If a magnetic field is sustained, there must be a current in a closed circuit or loop, implying some energy has been spent in creating the field. If this energy is not dissipated via the circuit's resistance, it is stored in the field.
Take an ideal inductor with zero resistance. Although it's practically impossible, assume that the coil's resistance is so small that it is practically negligible. The loss of the field's energy to dissipate thermal energy (or heat) is thus negligible.
The energy...
Potential Due to a Magnetized Object01:24

Potential Due to a Magnetized Object

Magnetic dipoles in magnetic materials are aligned when placed under an external magnetic field. For paramagnets and ferromagnets, dipole alignment occurs in the direction of the magnetic field. However, the dipoles align opposite to the field in the case of diamagnets. This state of magnetic polarization due to the external field is called magnetization. Magnetization is defined as the dipole moment per unit volume. It plays a similar role to polarization in electrostatics.
The vector...
Magnetic Susceptibility and Permeability01:31

Magnetic Susceptibility and Permeability

In linear magnetic materials, like paramagnets and diamagnets, magnetization is proportional to the magnetic field intensity. The constant of proportionality, a dimensionless number, is called magnetic susceptibility. The value of the susceptibility depends on the type of material.
When diamagnetic materials are placed under an external magnetic field, the moments opposite to the field are induced. Hence, the susceptibility for diamagnets has a minimal negative value of 10-5–10-6. Since...
Paramagnetism01:30

Paramagnetism

Paramagnets are materials with unpaired electrons that possess a finite magnetic moment. In the absence of a magnetic field, these moments are randomly oriented, and thus the net moment is zero. Under an external field, a torque acting on the moments tends to align them along the field's direction. However, the random thermal motion of electrons produces a torque opposite to the external field and tries to disorient the moments. These two competing effects align only a few moments along the...

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Updated: Jun 19, 2026

Magnetically Induced Rotating Rayleigh-Taylor Instability
06:42

Magnetically Induced Rotating Rayleigh-Taylor Instability

Published on: March 3, 2017

Finite dissipation and intermittency in magnetohydrodynamics.

P D Mininni1, A Pouquet

  • 1Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires and CONICET, Ciudad Universitaria, 1428 Buenos Aires, Argentina.

Physical Review. E, Statistical, Nonlinear, and Soft Matter Physics
|October 2, 2009
PubMed
Summary

Numerical simulations reveal that magnetohydrodynamic (MHD) turbulence dissipation approaches a constant at high Reynolds numbers, suggesting fast reconnection events in solar environments. MHD flow intermittency is stronger than fluid turbulence, with distinct velocity and magnetic field exponents.

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Ultrasound Velocity Measurement in a Liquid Metal Electrode
08:41

Ultrasound Velocity Measurement in a Liquid Metal Electrode

Published on: August 5, 2015

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Last Updated: Jun 19, 2026

Magnetically Induced Rotating Rayleigh-Taylor Instability
06:42

Magnetically Induced Rotating Rayleigh-Taylor Instability

Published on: March 3, 2017

Ultrasound Velocity Measurement in a Liquid Metal Electrode
08:41

Ultrasound Velocity Measurement in a Liquid Metal Electrode

Published on: August 5, 2015

Area of Science:

  • Plasma physics
  • Astrophysics
  • Computational fluid dynamics

Background:

  • Turbulence plays a crucial role in energy transfer and dissipation in astrophysical plasmas.
  • Understanding magnetohydrodynamic (MHD) turbulence is key to explaining phenomena like solar flares and coronal heating.
  • Previous studies suggest intermittency in MHD flows, but detailed scaling laws and dissipation behavior at high Reynolds numbers require further investigation.

Purpose of the Study:

  • To analyze the behavior of decaying magnetohydrodynamic (MHD) turbulence using high-resolution numerical simulations.
  • To investigate the dissipation characteristics and intermittency of MHD flows at elevated Reynolds numbers.
  • To explore the spectral scaling laws governing MHD turbulence.

Main Methods:

  • Numerical simulations of decaying MHD turbulence were performed up to a grid resolution of 1536^3.
  • The simulations covered Taylor Reynolds numbers up to approximately 1200.
  • Data analysis focused on the peak dissipation phase, examining structure functions and spectral properties.

Main Results:

  • Dissipation in MHD turbulence appears to asymptote to a constant value as the Reynolds number increases.
  • Intermittency in MHD flows is confirmed to be stronger than in fluid turbulence.
  • A measurable difference was found between the anomalous exponents of the velocity and magnetic fields.

Conclusions:

  • The results support the possibility of fast magnetic reconnection events in the solar environment at very high Reynolds numbers.
  • The observed differences in velocity and magnetic field intermittency align with recent solar wind observations.
  • The study provides insights into the spectral scaling laws governing MHD turbulence, contributing to our understanding of plasma dynamics.