Jove
Visualize
Contáctanos

Videos de Conceptos Relacionados

Faraday Disk Dynamo01:23

Faraday Disk Dynamo

2.4K
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...
2.4K
Atomic Nuclei: Nuclear Relaxation Processes01:23

Atomic Nuclei: Nuclear Relaxation Processes

697
In the absence of an external magnetic field, nuclear spin states are degenerate and randomly oriented. When a magnetic field is applied, the spins begin to precess and orient themselves along (lower energy) or against (higher energy) the direction of the field. At equilibrium, a slight excess population of spins exists in the lower energy state. Because the direction of the magnetic field is fixed as the z-axis,  the precessing magnetic moments are randomly oriented around the z-axis.
697
Momentum And Radiation Pressure01:20

Momentum And Radiation Pressure

2.1K
An object absorbing an electromagnetic wave would experience a force in the direction of propagation of the wave. This force occurs because electromagnetic waves contain and transport momentum. The force accounts for the wave's radiation pressure exerted on the object. Maxwell's prediction was confirmed in 1903 by Nichols and Hull by precisely measuring radiation pressures with a torsion balance. The measuring instrument had mirrors suspended from a fiber kept inside a glass container.
2.1K
Radiation Pressure: Problem Solving01:09

Radiation Pressure: Problem Solving

425
The radiation pressure applied by an electromagnetic wave on a perfectly absorbing surface equals the energy density of the wave. The wave's momentum also gets transferred to the surface when an electromagnetic wave is entirely absorbed by it. The rate at which momentum is transmitted to an absorbing surface perpendicular to the propagation direction equals the force on the surface.
The average value of the rate of momentum transfer divided by the absorbing area represents the average force...
425
Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

1.1K
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...
1.1K
Atomic Nuclei: Nuclear Spin State Population Distribution01:14

Atomic Nuclei: Nuclear Spin State Population Distribution

1.1K
Near absolute zero temperatures, in the presence of a magnetic field, the majority of nuclei prefer the lower energy spin-up state to the higher energy spin-down state. As temperatures increase, the energy from thermal collisions distributes the spins more equally between the two states. The Boltzmann distribution equation gives the ratio of the number of spins predicted in the spin −½ (N−) and spin +½ (N+) states.
1.1K

También podría leer

Artículos Relacionados

Artículos vinculados a este trabajo por autores compartidos, revista y gráfico de citas.

Ordenar por
Same author

Thermoelectricity at a gallium-mercury liquid metal interface.

Proceedings of the National Academy of Sciences of the United States of America·2024
Ver todos los artículos relacionados
JoVE
x logofacebook logolinkedin logoyoutube logo
ACERCA DE JoVE
Visión GeneralLiderazgoBlogCentro de Ayuda JoVE
AUTORES
Proceso de PublicaciónConsejo EditorialAlcance y PolíticasRevisión por ParesPreguntas FrecuentesEnviar
BIBLIOTECARIOS
TestimoniosSuscripcionesAccesoRecursosConsejo Asesor de BibliotecasPreguntas Frecuentes
INVESTIGACIÓN
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchivo
EDUCACIÓN
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualCentro de Recursos para ProfesoresSitio de Profesores
Términos y Condiciones de Uso
Política de Privacidad
Políticas

Video Experimental Relacionado

Updated: Aug 13, 2025

Magnetically Induced Rotating Rayleigh-Taylor Instability
06:42

Magnetically Induced Rotating Rayleigh-Taylor Instability

Published on: March 3, 2017

9.6K

Spin-down por la acción de la dínamo en las capas estelares radiativas simuladas

Ludovic Petitdemange1, Florence Marcotte2, Christophe Gissinger3,4

  • 1Laboratoire d'Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA), Observatoire de Paris, Paris Sciences & Lettres (PSL) Research University, French National Centre for Scientific Research (CNRS), Sorbonne Université, Paris, France.

Science (New York, N.Y.)
|January 19, 2023
PubMed
Resumen

La dinámica de rotación estelar interna es crucial para la evolución de las estrellas, pero se entiende mal. Nuestras simulaciones revelan un mecanismo de dínamo magnético que mejora el transporte del momento angular y genera fuertes campos magnéticos internos en las estrellas.

Más Videos Relacionados

High-Temperature and High-Pressure In situ Magic Angle Spinning Nuclear Magnetic Resonance Spectroscopy
08:55

High-Temperature and High-Pressure In situ Magic Angle Spinning Nuclear Magnetic Resonance Spectroscopy

Published on: October 9, 2020

5.7K
Evolution of Staircase Structures in Diffusive Convection
07:28

Evolution of Staircase Structures in Diffusive Convection

Published on: September 5, 2018

6.6K

Videos de Experimentos Relacionados

Last Updated: Aug 13, 2025

Magnetically Induced Rotating Rayleigh-Taylor Instability
06:42

Magnetically Induced Rotating Rayleigh-Taylor Instability

Published on: March 3, 2017

9.6K
High-Temperature and High-Pressure In situ Magic Angle Spinning Nuclear Magnetic Resonance Spectroscopy
08:55

High-Temperature and High-Pressure In situ Magic Angle Spinning Nuclear Magnetic Resonance Spectroscopy

Published on: October 9, 2020

5.7K
Evolution of Staircase Structures in Diffusive Convection
07:28

Evolution of Staircase Structures in Diffusive Convection

Published on: September 5, 2018

6.6K

Área de la Ciencia:

  • Astrofísica estelar
  • Magnetohidrodinámica
  • Física computacional

Sus antecedentes:

  • La evolución de las estrellas se rige por la dinámica de rotación interna, que afecta a los procesos de transporte y mezcla.
  • El origen de los campos magnéticos en los interiores estelares radiativos y su papel en el transporte del momento angular siguen sin estar claros.
  • Comprender el magnetismo estelar es clave para explicar las propiedades estelares observadas.

Objetivo del estudio:

  • Para investigar la generación de campos magnéticos en el interior estelar radiativo.
  • Explorar el papel de los campos magnéticos en el momento angular y el transporte de elementos químicos.
  • Identificar el mecanismo responsable de la acción del dínamo estelar en las zonas radiativas.

Principales métodos:

  • Simulaciones numéricas globales de los interiores estelares.
  • Análisis de las transiciones del flujo de fluidos de los estados laminares a los turbulentos.
  • Modelado de la generación y el transporte de campos magnéticos.

Principales resultados:

  • Se identificó una transición subcrítica del flujo laminar a la turbulencia, impulsada por la generación de dínamo magnético.
  • El dínamo simulado exhibe propiedades consistentes con el mecanismo del dínamo de Tayler-Spruit.
  • Se generan campos magnéticos toroidales fuertes y profundos y, posteriormente, son protegidos por las capas externas estelares.

Conclusiones:

  • El mecanismo de dinamo de Tayler-Spruit proporciona una explicación viable para el transporte de momento angular mejorado en las zonas radiativas estelares.
  • Este mecanismo puede generar campos magnéticos internos significativos en las estrellas sin un campo magnético de superficie detectable.
  • Los hallazgos ofrecen información sobre la dinámica interna poco comprendida que influye en la evolución estelar.