Jove
Visualize
Contact Us
JoVE
x logofacebook logolinkedin logoyoutube logo
ABOUT JoVE
OverviewLeadershipBlogJoVE Help Center
AUTHORS
Publishing ProcessEditorial BoardScope & PoliciesPeer ReviewFAQSubmit
LIBRARIANS
TestimonialsSubscriptionsAccessResourcesLibrary Advisory BoardFAQ
RESEARCH
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchive
EDUCATION
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualFaculty Resource CenterFaculty Site
Terms & Conditions of Use
Privacy Policy
Policies

Related Concept Videos

Magnetic Field Lines01:19

Magnetic Field Lines

4.6K
The representation of magnetic fields by magnetic field lines is very useful in visualizing the strength and direction of the magnetic field. Each of the magnetic field lines forms a closed loop. The field lines emerge from the north pole (N), loop around to the south pole (S), and continue through the bar magnet back to the north pole.
Magnetic field lines follow several hard-and-fast rules:
4.6K
Faraday Disk Dynamo01:23

Faraday Disk Dynamo

2.7K
A Faraday disk dynamo is a DC generator, producing an emf that is constant in time. It consists of a conducting disk that rotates with a constant angular velocity in the magnetic field, perpendicular to the disk's plane. The rotation of the disk causes a change in magnetic flux, which induces an emf, causing opposite charges to develop on the rim and in the center of the disk. The polarity of the induced emf can be determined by the direction of the magnetic field and the direction of the...
2.7K
Fermi Level Dynamics01:12

Fermi Level Dynamics

380
The vacuum level denotes the energy threshold required for an electron to escape from a material surface. It is usually positioned above the conduction band of a semiconductor and acts as a benchmark for comparing electron energies within various materials.
Electron affinity in semiconductors refers to the energy gap between the minimum of its conduction band and the vacuum level and it is a critical parameter in determining how easily a semiconductor can accept additional electrons.
The work...
380
Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

1.2K
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...
1.2K
Magnetic Flux01:18

Magnetic Flux

3.9K
The magnetic flux measures the number of magnetic field lines passing through a given surface area. The SI unit for magnetic flux is the weber (Wb). Magnetic flux is a scalar quantity. It depends on three factors: the strength of the magnetic field B, the area through which the field lines pass, and the relative orientation of the field with the surface area.
Suppose a surface is divided into elements of area dA. For each element, the component of the magnetic field that is normal to the...
3.9K
Potential Due to a Magnetized Object01:24

Potential Due to a Magnetized Object

375
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...
375

You might also read

Related Articles

Articles linked to this work by shared authors, journal, and citation graph.

Sort by
Same author

Extremely active Sun from 1190 to 1220 in the Medieval Period: Intercomparison of historical records and tree-ring carbon-14.

Proceedings of the Japan Academy. Series B, Physical and biological sciences·2026
Same author

A galactic cosmic ray cavity in Earth-Moon space.

Science advances·2026
Same author

<i>In situ</i> Hybridization to Study the Pathogenicity of North American Avian Metapneumovirus Subtypes A and B in Turkeys.

Avian diseases·2026
Same author

Identification of a Novel Astrovirus Associated with Bovine Respiratory Disease.

Transboundary and emerging diseases·2025
Same author

Ischemic myelomalacia and closed spinal dysraphism in multiple finishing swine.

Veterinary pathology·2022
Same author

Polarized blazar X-rays imply particle acceleration in shocks.

Nature·2022
Same journal

Transport of Electrons in Tangled Magnetic Fields.

Space science reviews·2026
Same journal

The Solar Wind Electron (SWE) Instrument for the Interstellar Mapping and Acceleration Probe Mission.

Space science reviews·2026
Same journal

Inter-comparison of Mars Upper Atmosphere Neutral Density and Temperature Datasets from MAVEN.

Space science reviews·2026
Same journal

The Interstellar Mapping And Acceleration Probe High Energy (IMAP-Hi) Neutral Atom Imager.

Space science reviews·2026
Same journal

Origin and Evolution of the Galilean Satellites Within the Jovian System.

Space science reviews·2026
Same journal

The IMAP Magnetometer.

Space science reviews·2026
See all related articles

Related Experiment Video

Updated: Oct 15, 2025

Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
06:14

Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface

Published on: July 30, 2020

5.1K

Small-Scale Dynamic Aurora.

Ryuho Kataoka1,2, Christopher C Chaston3, David Knudsen4

  • 1National Institute of Polar Research, 10-3 Midori-cho, Tachikawa, Tokyo, 185-0031 Japan.

Space Science Reviews
|November 1, 2021
PubMed
Summary
This summary is machine-generated.

Small-scale dynamic auroras, like flickering auroras and vortex motions, result from complex interactions in Earth's magnetosphere. Understanding these phenomena involves studying dispersive Alfvén waves and plasma instabilities.

Keywords:
Auroral breakupAuroral phenomenaDispersive Alfven wavesFlickering auroraIonospheric Alfven resonatorIonospheric feedback instabilitiesMagnetosphere-ionosphere coupled region

More Related Videos

Method for Recording Broadband High Resolution Emission Spectra of Laboratory Lightning Arcs
07:51

Method for Recording Broadband High Resolution Emission Spectra of Laboratory Lightning Arcs

Published on: August 27, 2019

7.1K
Real-Time Monitoring of Aurora kinase A Activation using Conformational FRET Biosensors in Live Cells
06:29

Real-Time Monitoring of Aurora kinase A Activation using Conformational FRET Biosensors in Live Cells

Published on: July 30, 2020

3.2K

Related Experiment Videos

Last Updated: Oct 15, 2025

Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
06:14

Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface

Published on: July 30, 2020

5.1K
Method for Recording Broadband High Resolution Emission Spectra of Laboratory Lightning Arcs
07:51

Method for Recording Broadband High Resolution Emission Spectra of Laboratory Lightning Arcs

Published on: August 27, 2019

7.1K
Real-Time Monitoring of Aurora kinase A Activation using Conformational FRET Biosensors in Live Cells
06:29

Real-Time Monitoring of Aurora kinase A Activation using Conformational FRET Biosensors in Live Cells

Published on: July 30, 2020

3.2K

Area of Science:

  • Space Physics
  • Plasma Physics
  • Atmospheric Physics

Background:

  • Small-scale dynamic auroras exhibit spatial and temporal scales of a few kilometers and seconds, respectively.
  • These auroras reveal intricate interactions within the magnetosphere-ionosphere coupled system.

Purpose of the Study:

  • To summarize observed properties of small-scale dynamic auroras.
  • To review fundamental theories explaining these auroral phenomena.

Main Methods:

  • Observational data analysis of auroral structures.
  • Theoretical development and review of plasma physics concepts.

Main Results:

  • Detailed properties of flickering auroras, vortex motions, and filamentary structures are presented.
  • Key theories including dispersive Alfvén waves, plasma instabilities, ionospheric feedback instabilities, and the ionospheric Alfvén resonator are summarized.

Conclusions:

  • Small-scale dynamic auroras are crucial for understanding magnetosphere-ionosphere coupling.
  • The reviewed theories provide a framework for explaining the complex dynamics observed in auroras.