Name: radiation pressure in light and comets
Uploaded: 2023-04-30T12:46:50.000Z
Duration: 1 min 20 s
Channel: JoVE

K12 Standards

Pennsylvania State Academic Standards

9-12

Earth and Space Science

Earth's Systems

3.3.9-12.H

Momentum And Radiation Pressure

Las ondas electromagnéticas transportan impulso mientras viajan por el espacio. La densidad de momento correspondiente se expresa en términos de la magnitud del vector de Poynting y la velocidad de la luz.
Sustituyendo el volumen ocupado por la onda que pasa a través de un área en un corto intervalo de tiempo, se puede obtener el caudal de momento por unidad de área.
La tasa promedio de transferencia de momento por unidad de área se obtiene reemplazando el valor promedio del vector de Poynting por la intensidad.
Debido a la transferencia de momento, las ondas electromagnéticas ejercen presión sobre la superficie, conocida como presión de radiación.
Ahora, la tasa promedio de cambio de momento es igual a la fuerza promedio y la fuerza por unidad de área es la presión de radiación.
Por lo tanto, la presión de radiación es directamente proporcional a la intensidad de la onda.
Si la superficie absorbe perfectamente la onda electromagnética, el momento correspondiente también se transfiere completamente a la superficie.
Para una superficie perfectamente reflectante, el cambio de momento será el doble. Por lo tanto, la presión de radiación también se duplica.

<ol>
	<li>OpenStax. (2019). Física Universitaria Vol. 2. [Versión web]. Obtenido de <a href="https://openstax.org/books/university-physics-volume-2/pages/16-4-momentum-and-radiation-pressure">16.4 Momento y Presión de Radiación - Física Universitaria Volumen 2 | OpenStax</a></li>
</ol>

impulso y presión radiante

Un objeto que absorbe una onda electromagnética experimentaría una fuerza en la dirección de propagación de la onda. Esta fuerza ocurre porque las ondas electromagnéticas contienen y transportan impulso. La fuerza representa la presión radiante de la onda ejercida sobre el objeto. La predicción de Maxwell fue confirmada en 1903 por Nichols y Hull al medir con precisión las presiones radiantes con un equilibrio de torsión. El instrumento de medición tenía espejos suspendidos de una fibra mantenida dentro de un recipiente de vidrio. Nichols y Hull obtuvieron una ligera desviación medible de los espejos al iluminar uno de ellos. A partir de la desviación medida, calcularon la fuerza desequilibrada sobre el espejo y obtuvieron una coincidencia con el valor predicho de la fuerza. La presión radiante aplicada por una onda electromagnética en una superficie perfectamente absorbente resulta ser igual a la densidad de energía de la onda. Supongamos que el material es perfectamente reflectivo y las ondas electromagnéticas inciden perpendicularmente a la superficie. En ese caso, la presión ejercida es el doble porque la dirección del impulso se invierte al reflejarse. La presión radiante juega un papel en la explicación de muchos fenómenos astronómicos observados, incluyendo la apariencia de los cometas. Cuando un cometa se acerca al Sol, se calienta y su superficie, compuesta de gases congelados y partículas de roca y polvo, se evapora. La coma del cometa es la zona turbia a su alrededor compuesta por los gases y el polvo. Algunos de los gases y el polvo forman colas cuando abandonan el cometa. La cola iónica está compuesta principalmente por gases ionizados. Estos iones interactúan electromagnéticamente con el viento solar, una corriente continua de partículas cargadas emitidas por el Sol. La fuerza del viento solar sobre los gases ionizados es lo suficientemente fuerte como para que la cola iónica casi siempre apunte directamente lejos del Sol. La segunda cola está compuesta por partículas de polvo. Debido a que la cola de polvo es eléctricamente neutral, no interactúa con el viento solar. Sin embargo, esta cola se ve afectada por la presión radiante producida por la luz del Sol. Aunque relativamente pequeña, esta presión es lo suficientemente fuerte como para que la cola de polvo se desplace de la trayectoria del cometa.

Impulso Y Presión Radiante

Un objeto que absorbe una onda electromagnética experimentaría una fuerza en la dirección de propagación de la onda. Esta fuerza se produce porque ...

Education

Educación

JoVE Core

Physics

Física

Unit 1

Unidad 1

Electromagnetic Waves

Ondas electromagnéticas

KEY TERMS AND CONCEPTS

TÉRMINOS Y CONCEPTOS CLAVE

radiation pressure in light and comets

Radiation pressure is the force that electromagnetic waves can exert on matter. It appears because light carries momentum, so an object that absorbs a wave feels a push in the direction the wave travels. This same force helps explain why sunlight can affect small particles in space.

Maxwell predicted radiation pressure, and Nichols and Hull confirmed it in 1903. They used a torsion balance with mirrors suspended from a fiber inside a glass container. When they shone light on one mirror, the mirrors shifted slightly. From that tiny deflection, they calculated the unbalanced force and found agreement with the predicted value.

The size of the pressure depends on the surface. For a perfectly absorbing surface, the radiation pressure equals the energy density of the wave. For a perfectly reflecting surface with the wave hitting straight on, the pressure is twice as large because the light reverses momentum when it reflects.

Radiation pressure also helps explain comet tails. When a comet nears the Sun, it warms up and releases frozen gases, rock, and dust. This forms a coma, which is the hazy cloud around the comet, and it can also create tails.

The ion tail is made mostly of ionized gases. These ions interact with the solar wind, a stream of charged particles from the Sun, and the tail usually points away from the Sun. The dust tail is different. It contains neutral dust, so it does not respond to the solar wind. Instead, sunlight’s radiation pressure pushes the dust tail away from the comet’s path.

Radiation Pressure in Light and Comets

electromagnetic waves

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Maxwell’s equations explain how electric and magnetic fields work together to create electromagnetic waves. James Clerk Maxwell brought together the ideas of Oersted, Coulomb, Gauss, and Faraday and built a single theory of electromagnetism. Together with the Lorentz force law, his equations describe the laws of electricity and magnetism. A key part of Maxwell’s work is the symmetry in the equations. Faraday’s law shows that a changing magnetic field produces an electric field. Maxwell added...

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momentum and radiation pressure

Radiation pressure is the force that electromagnetic waves can exert on matter. It appears because light carries momentum, so an object that absorbs a wave feels a push in the direction the wave travels. This same force helps explain why sunlight can affect small particles in space. Maxwell predicted radiation pressure, and Nichols and Hull confirmed it in 1903. They used a torsion balance with mirrors suspended from a fiber inside a glass container. When they shone light on one mirror, the...

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Radiation Pressure in Light and Space

Radiation pressure is the push that light can exert on matter. When an electromagnetic wave is completely absorbed by a surface, its energy density is transferred as momentum to that surface. The rate of momentum transfer on a surface perpendicular to the wave gives the force, and the force per unit area is the radiation pressure. A perfectly absorbing surface receives this pressure directly from the incoming wave. If the surface is perfectly reflecting, such as a metal surface, and the light...

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key terms and concepts

Explore how light carries momentum, creates radiation pressure, and was measured by Nichols and Hull. See how it helps shape comet tails.

Radiation Pressure in Light and Comets | JoVE K12

physics

JoVE Core Física presenta la teoría y la aplicación de conceptos físicos fundamentales, como la cinemática, dinámica, mecánica de fluidos, estática, ondas y acústica, mediante animaciones audiovisuales concisas y fáciles de entender. Además, los vídeos de científicos en acción muestran la aplicación de los conceptos relacionados en experimentos de investigación clásicos y originales, realizados en laboratorios de todo el mundo.

Weather and Climate

3.3.9-12.E

Physical Science

Waves and Electromagnetic Radiation

3.2.9-12.V

Louisiana Student Standards for Science

High School

Earth Science

Earth’s Systems

HS-ESS2-1

HS-ESS2-4

waves-and-their-applications-in-technologies-for-information-transfer

Waves And Their Applications In Technologies For Information Transfer

HS-PS4-1

Virginia  Standards of Learning

HIgh School

PS.7

PS.7.a

Alabama Course of Study Science

Waves and Their Applications in Technologies for Information Transfer

9-12.PS.2.2.e

9-12.P.3.7.c

Florida Department of Education

SC.912.P.10

SC.912.P.10.19

south-carolina-college-and-career-ready-science-standards

South Carolina College and Career Ready Science Standards

P-PS4-4

Earth and Space Science (ESS)

Earth’s Place in the Universe

E-ESS1-2.

E-ESS2-4.

new-york-state-science-learning-standards

New York State Science Learning Standards

HS. Waves and Electromagnetic Radiation

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3.3.9-12.L

Radiation Pressure in Light and Comets

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