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Videos de Conceptos Relacionados

Radiation Pressure: Problem Solving01:09

Radiation Pressure: Problem Solving

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 per...
Momentum And Radiation Pressure01:20

Momentum And Radiation Pressure

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. Nichols...
Schwarzschild Radius and Event Horizon01:21

Schwarzschild Radius and Event Horizon

No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape velocity with the...
Radiation: Applications01:17

Radiation: Applications

The average temperature of Earth is the subject of much current discussion. Earth is in radiative contact with both the Sun and dark space; it receives almost all its energy from the radiation of the Sun and reflects some of it into outer space. Dark space is very cold, about 3 K, so Earth radiates energy into it. For instance, heat transfer occurs from soil and grasses, the rate of which can be so rapid that frost can occur on clear summer evenings, even in warm latitudes.
The average...
Absorption of Radiation01:05

Absorption of Radiation

The rate of heat transfer by emitted radiation is described by the Stefan-Boltzmann law of radiation:
Electromagnetic Waves in Matter01:30

Electromagnetic Waves in Matter

Electromagnetic waves can travel in the vacuum as well as in matter. For example light, which is an electromagnetic wave, can travel through air, water, or glass.
Consider the electromagnetic wave passing through a dielectric medium. In such a case, Maxwell's equations get modified. In Ampere's law, ε0 , the dielectric permittivity of free space is replaced with ε, the permittivity of dielectric. Also, the vacuum permeability μ0 is replaced by the permeability of the medium, μ.
Furthermore, the...

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Video Experimental Relacionado

Updated: Jul 11, 2026

Scattering And Absorption of Light in Planetary Regoliths
11:34

Scattering And Absorption of Light in Planetary Regoliths

Published on: July 1, 2019

El registro de rayos cósmicos en la materia del sistema solar.

R C Reedy, J R Arnold, D Lal

    Science (New York, N.Y.)
    |January 14, 1983
    PubMed
    Resumen

    Los rayos cósmicos que interactúan con los objetos del sistema solar revelan su historia. El análisis de nucleidos y huellas de partículas muestra variaciones pasadas en los flujos de rayos cósmicos durante millones de años.

    Área de la Ciencia:

    • Física de los rayos cósmicos Física de los rayos cósmicos
    • Ciencias planetarias Ciencias planetarias.
    • La astrofísica nuclear es una astrofísica nuclear.

    Sus antecedentes:

    • Los núcleos energéticos en los rayos cósmicos interactúan con los cuerpos del sistema solar como los meteoritos, la Luna y los planetas.
    • Estas interacciones producen nucleidos y huellas de núcleos pesados dentro de los materiales objetivo.

    Objetivo del estudio:

    • Para investigar la información contenida en los nucleidos y las huellas producidas por los rayos cósmicos.
    • Para entender la historia de los objetos del sistema solar y las variaciones en los flujos de partículas.
    • Para analizar historias complejas de exposición a rayos cósmicos de muestras lunares y meteoritos.

    Principales métodos:

    • Análisis de nucleidos y huellas de núcleos pesados en materiales extraterrestres.

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  • Reconstrucción de las historias de exposición a rayos cósmicos.
  • Investigación de la erosión, jardinería, fragmentación y cambios orbitales que afectan a las muestras.

    • Principales resultados:

    • Las interacciones de rayos cósmicos proporcionan registros históricos detallados de los objetos del sistema solar.
    • La evidencia sugiere variaciones temporales y espaciales en los flujos de partículas de rayos cósmicos.
    • Historias complejas de exposición son comunes en muestras lunares y meteoritos debido a varios procesos.

    Conclusiones:

    • Las historias de exposición a rayos cósmicos son cruciales para comprender la evolución del sistema solar.
    • Los flujos de partículas solares pasados muestran variaciones en escalas de tiempo de 10^4 a 10^7 años.
    • Se justifica una mayor investigación sobre las variaciones del flujo de los rayos cósmicos galácticos.