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

Faraday Disk Dynamo01:23

Faraday Disk Dynamo

2.2K
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...
2.2K
Divergence and Curl of Magnetic Field01:26

Divergence and Curl of Magnetic Field

2.9K
The magnetic field due to a volume current distribution given by the Biot–Savart Law can be expressed as follows:
2.9K
Maxwell-Boltzmann Distribution: Problem Solving01:20

Maxwell-Boltzmann Distribution: Problem Solving

1.5K
Individual molecules in a gas move in random directions, but a gas containing numerous molecules has a predictable distribution of molecular speeds, which is known as the Maxwell-Boltzmann distribution, f(v).
This distribution function f(v) is defined by saying that the expected number N (v1,v2) of particles with speeds between v1 and v2 is given by
1.5K
Differential Form of Maxwell's Equations01:17

Differential Form of Maxwell's Equations

459
James Clerk Maxwell (1831–1879) was one of the significant contributors to physics in the nineteenth century. He is probably best known for having combined existing knowledge of the laws of electricity and the laws of magnetism with his insights to form a complete overarching electromagnetic theory, represented by Maxwell's equations. The four basic laws of electricity and magnetism were discovered experimentally through the work of physicists such as Oersted, Coulomb, Gauss, and...
459
Fast Decoupled and DC Powerflow01:24

Fast Decoupled and DC Powerflow

182
The fast decoupled power flow method addresses contingencies in power system operations, such as generator outages or transmission line failures. This method provides quick power flow solutions, essential for real-time system adjustments. Fast decoupled power flow algorithms simplify the Jacobian matrix by neglecting certain elements, leading to two sets of decoupled equations:
182
Maxwell's Equation Of Electromagnetism01:29

Maxwell's Equation Of Electromagnetism

3.1K
James Clerk Maxwell (1831–1879) was one of the major contributors to physics in the nineteenth century. Although he died young, he made major contributions to the development of the kinetic theory of gases, to the understanding of color vision, and to understanding the nature of Saturn's rings. He is probably best known for having combined existing knowledge on the laws of electricity and magnetism with his insights into a complete overarching electromagnetic theory, which is...
3.1K

You might also read

Related Articles

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

Sort by
Same author

A modelling study to explore the effects of regional socio-economics on the spreading of epidemics.

Journal of computational social science·2024
Same author

Supernova dust destruction in the magnetized turbulent ISM.

Nature communications·2024
Same journal

Magnetic, thermal and rotational evolution of isolated neutron stars.

Living reviews in computational astrophysics·2026
Same journal

Simulations of multi-phase gas in and around galaxies.

Living reviews in computational astrophysics·2026
Same journal

Spectral synthesis techniques for supernovae and kilonovae.

Living reviews in computational astrophysics·2025
Same journal

Neutrino transport in general relativistic neutron star merger simulations.

Living reviews in computational astrophysics·2023
Same journal

Well-balanced methods for computational astrophysics.

Living reviews in computational astrophysics·2022
Same journal

Simulations of cosmic ray propagation.

Living reviews in computational astrophysics·2021
See all related articles

Related Experiment Video

Updated: Jun 22, 2025

A Rapid Method for Modeling a Variable Cycle Engine
04:58

A Rapid Method for Modeling a Variable Cycle Engine

Published on: August 13, 2019

7.5K

Computational approaches to modeling dynamos in galaxies.

Maarit J Korpi-Lagg1,2,3, Mordecai-Mark Mac Low4, Frederick A Gent1,2,5,6

  • 1Astroinformatics, Department of Computer Science, Aalto University, P.O. Box 15400, 00076 Espoo, Finland.

Living Reviews in Computational Astrophysics
|July 5, 2024
PubMed
Summary
This summary is machine-generated.

Galactic magnetic fields are generated by turbulent dynamos in early galaxies. Large-scale dynamos then amplify these fields to observed strengths in later galaxies, influencing galactic evolution.

Keywords:
DynamoGalaxyInterstellar mediumMagnetic fieldsNumerical methods

More Related Videos

Computational Modeling of Retinal Neurons for Visual Prosthesis Research - Fundamental Approaches
10:50

Computational Modeling of Retinal Neurons for Visual Prosthesis Research - Fundamental Approaches

Published on: June 21, 2022

1.7K
Methods for Measuring the Orientation and Rotation Rate of 3D-printed Particles in Turbulence
12:34

Methods for Measuring the Orientation and Rotation Rate of 3D-printed Particles in Turbulence

Published on: June 24, 2016

10.1K

Related Experiment Videos

Last Updated: Jun 22, 2025

A Rapid Method for Modeling a Variable Cycle Engine
04:58

A Rapid Method for Modeling a Variable Cycle Engine

Published on: August 13, 2019

7.5K
Computational Modeling of Retinal Neurons for Visual Prosthesis Research - Fundamental Approaches
10:50

Computational Modeling of Retinal Neurons for Visual Prosthesis Research - Fundamental Approaches

Published on: June 21, 2022

1.7K
Methods for Measuring the Orientation and Rotation Rate of 3D-printed Particles in Turbulence
12:34

Methods for Measuring the Orientation and Rotation Rate of 3D-printed Particles in Turbulence

Published on: June 24, 2016

10.1K

Area of Science:

  • Astrophysics
  • Cosmic Magnetism
  • Galaxy Formation

Background:

  • Galaxies possess significant magnetic fields, with total strengths around 15 microgauss.
  • These fields, comprising coherent large-scale components and strong turbulent fluctuations, are dynamically important.
  • Key questions concern the origin, influence on galaxy evolution, and physical processes involving galactic magnetic fields.

Purpose of the Study:

  • To review numerical modeling techniques for magnetized galactic flows.
  • To investigate the physical mechanisms responsible for generating and sustaining galactic magnetic fields.
  • To understand the role of magnetic fields in galaxy formation and evolution.

Main Methods:

  • Review of numerical modeling techniques for magnetized flows in galaxies.
  • Analysis of results from simulations of turbulent dynamos (small-scale and large-scale).
  • Comparison of simulation outputs with observational data (e.g., Faraday rotation, polarization).

Main Results:

  • Small-scale turbulent dynamos likely generate magnetic fields in the first galaxies on short timescales.
  • These dynamos saturate at field strengths below equipartition with turbulence.
  • Large-scale dynamos in rotating galactic disks amplify fields to observed strengths in low-redshift galaxies, consistent with observations.

Conclusions:

  • Galactic magnetic field generation involves a two-stage dynamo process: initial small-scale dynamo followed by large-scale dynamo action.
  • The combined dynamo action explains the observed magnetic field strengths and structures in galaxies.
  • Challenges remain in scaling numerical models to realistic astrophysical conditions.