Name: radiation pressure in light and space
Uploaded: 2023-09-18T17:11:21.000Z
Duration: 1 min 9 s
Channel: JoVE

K12 Standards

north-carolina-k-12-science-standard-course-of-study

NC K-12 Science Standard Course of Study

9-12

Earth and Environmental Science

Earth's Place in the Universe

ESS.EES.1.4

Radiation Pressure: Problem Solving

Pensemos en un satélite en órbita alrededor de la Tierra. Su distancia al sol es de 1,5 X 1011 metros. El sol irradia con una potencia media de 3,8 X 1026 vatios.
Si sus paneles colectores solares tienen un área total de 20 metros cuadrados, ¿cuál sería la presión de radiación sobre los paneles solares y la fuerza debida a ella?
La intensidad de la radiación solar es igual a la potencia solar media por unidad de superficie. Por lo tanto, su valor en el satélite es de 1,3 X 103 vatios por metro cuadrado.
Suponiendo que los paneles solares absorben completamente toda la luz solar incidente, la presión de radiación sobre los paneles solares es igual a la intensidad de la radiación solar sobre la velocidad de la luz, que es de 4,3 X 10-6 newtons por metro cuadrado.
La fuerza de radiación es el producto de la presión de radiación y el área de los paneles solares. Su valor se calcula en 8,6 X 10-5 newtons.

<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">https://openstax.org/books/university-physics-volume-2/pages/16-4-momentum-and-radiation-pressure</a>; Sección 16.4; páginas 719-721.</li>
	<li>Young, H.D y Freedman, R.A. (2012). Física Universitaria con Física Moderna. San Francisco, CA: Pearson; Sección 32.4; páginas 1068-1069.</li>
</ol>

presión radiativa: resolución de problemas

La presión radiativa aplicada por una onda electromagnética en una superficie perfectamente absorbente es igual a la densidad de energía de la onda. El momento de la onda también se transfiere a la superficie cuando una onda electromagnética es completamente absorbida por ella. La rapidez con la que se transmite el momento a una superficie absorbente perpendicular a la dirección de propagación es igual a la fuerza sobre la superficie. El valor promedio de la tasa de transferencia de momento dividida por el área absorbente representa la fuerza promedio por unidad de área o presión radiativa debido a la onda. Si el material es perfectamente reflectante, como una superficie metálica, y la incidencia es normal a la superficie, entonces la presión ejercida se duplica porque la dirección del momento se invierte al reflejarse. La luz solar ejerce una presión radiativa mucho más fuerte dentro del sol que en la Tierra. La presión radiativa dentro de las estrellas que son significativamente más masivas y brillantes que el sol es tan alta que aumenta considerablemente la presión interna del gas, evitando que estas estrellas colapsen debido a su propia gravedad. A veces, la presión radiativa de las estrellas puede afectar significativamente el material en su inmediata cercanía. La presión radiativa juega un papel en la explicación de muchos otros fenómenos astronómicos observados, incluida la apariencia de los cometas. Cuando un cometa se acerca al sol, se calienta y su superficie comienza a evaporarse. Algunos de los gases y el polvo forman colas cuando abandonan el cometa. Un cometa tiene dos colas: la primera es la cola de iones, compuesta principalmente por gases ionizados. Estos iones interactúan electromagnéticamente con el viento solar. La fuerza del viento solar sobre los gases ionizados es lo suficientemente fuerte como para que la cola de iones 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 neutra, no interactúa con el viento solar. Sin embargo, esta cola se ve afectada por la presión radiativa producida por la luz del sol. Aunque bastante pequeña, esta presión es lo suficientemente fuerte como para hacer que la cola de polvo se desplace de la trayectoria del cometa.

Presión radiativa: Resolución de problemas

La presión de radiación aplicada por una onda electromagnética sobre una superficie perfectamente absorbente es igual a la densidad de energía de la onda. El impulso de la ola ...

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 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 strikes it straight on, the pressure doubles. That happens because the momentum changes direction after reflection.

Radiation pressure is much stronger inside the sun than it is on Earth. In stars that are more massive and brighter than the sun, it can greatly increase the internal gas pressure. This extra pressure helps keep those stars from collapsing under their own gravity.

Radiation pressure also helps explain comet tails. As a comet moves close to the sun, it warms up and its surface begins to evaporate. Gas and dust escape and form tails.

A comet has two tails. The ion tail is made mainly of ionized gas, and it interacts with the solar wind. That force is strong enough that the ion tail usually points directly away from the sun. The dust tail is electrically neutral, so it does not interact with the solar wind. Instead, sunlight pushes on it through radiation pressure, and this small force can make the dust tail bend away from the comet’s path.

Radiation Pressure in Light and Space

electromagnetic waves

Maxwell’s Equations Behind EM Waves

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...

generating electromagnetic radiations

Hertz's Spark Gaps and Radio Waves

Heinrich Hertz used sparks and tuned circuits to show that electromagnetic waves could be produced in the lab. Starting in 1887, the German physicist ran experiments that confirmed electromagnetic waves exist and travel at the speed of light. Hertz built an alternating-current RLC circuit. RLC stands for resistor, inductor, and capacitor. The circuit was set to a known resonant frequency and connected to a loop of wire. High voltage across the gap in the loop created sparks. Those sparks gave...

the electromagnetic spectrum

Electromagnetic Waves in Everyday Technology

Electromagnetic waves are grouped by wavelength and frequency. This set of waves is called the electromagnetic spectrum. It includes radio waves, microwaves, infrared, visible light, X-rays, and gamma rays. Radio waves have wavelengths from millimeters to kilometers. They are often used for audio communication, such as radios. In many cases, they come from alternating current in the wires of a broadcast antenna. Radio waves also carry AM and FM radio, cellular phone signals, and TV signals. <br...

electromagnetic wave equation

How Maxwell Linked Light to Waves

Maxwell's equations show how electric and magnetic fields behave in a vacuum, or empty space. They are written as differential equations and describe fields created by source charges, whether the charges are still or moving. These fields also act on a test charge, and its motion can be found with the right boundary conditions. The key question in empty space is what happens when there are no source charges. In the vacuum form of Maxwell's four equations, the first-order partial differential...

plane electromagnetic waves i

Transverse Fields in Electromagnetic Waves

Electromagnetic waves are made of electric and magnetic fields that move through space together. Maxwell's equations predict these waves, and they can travel in free space without a medium. The electric field acts on a stationary charge, while the magnetic field acts on a moving charge. For a wave traveling along the x-axis, the fields are written as Ey(x, t) and Bz(x, t). In free space, there are no free charges or currents, so the charge enclosed and current terms in Maxwell's equations are...

plane electromagnetic waves ii

Faraday’s Law in a Plane Wave

Faraday’s law can be used to link the electric and magnetic fields in a plane electromagnetic wave. Here, the wavefront moves in the x-direction at a constant speed. The goal is to show how the field strengths must be related for the wave to stay consistent with Faraday’s law. To apply the law, a rectangle of width a is placed with its area vector in the positive z-direction. The line integral is taken counterclockwise around the rectangle. One side lies outside the wavefront, so the electric...

propagation speed of electromagnetic waves

propagation-speed-of-electromagnetic-waves

Maxwell’s Equations and Light Speed

Electromagnetic waves follow Ampere’s law when there is no conduction current. A plane wavefront moves in the positive x-direction. To analyze it, a rectangle is placed in the xz-plane with its area vector pointing in the positive y-direction. The line integral around the rectangle is taken counterclockwise. The magnetic field is zero on some sides and perpendicular on others. It is parallel to one side, and that side gives a non-zero contribution to the integral. Because the left side of...

electromagnetic waves in matter

How Light Slows in Materials

Electromagnetic waves can travel through matter as well as through vacuum. Light is one example. It can move through air, water, or glass. When an electromagnetic wave passes through a dielectric medium, the equations that describe it change. In Ampere's law, the permittivity of free space, ε0, is replaced by the permittivity of the dielectric, ε. The vacuum permeability, μ0, is also replaced by the permeability of the medium, μ. The wave speed c in vacuum is then replaced by a lower speed, v,...

energy carried by electromagnetic waves

How EM Waves Transfer Energy

Electromagnetic waves transfer energy through their electric and magnetic fields. This energy can be easy to notice, like the warmth from the summer sun, or harder to feel, like the energy in gamma rays that can damage living cells. The fields in an electromagnetic wave can exert forces on charges in a system. They can move those charges and do work on them. Even if a wave is not absorbed right away, it still carries energy away from its source. If some of the wave energy is absorbed, the...

intensity of electromagnetic waves

Poynting Vector and Light Intensity

The Poynting vector describes the energy flux of an electromagnetic wave. It tells how much energy passes through a unit area in a unit time at a specific moment. For a plane electromagnetic wave moving along the x-axis, the energy flux depends on the peak electric field E0 and the peak magnetic field B0. For high-frequency waves, the energy flux changes very quickly with time. Visible light has a frequency on the order of 10^14 Hz, so its energy flux varies too fast to track directly. Most...

momentum and radiation pressure

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...

radiation pressure: problem solving

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...

standing electromagnetic waves

Electromagnetic Wave Reflection at Conductors

Electromagnetic waves can reflect from a conductor or a dielectric. When the reflected wave combines with the incoming wave, the result is a standing electromagnetic wave. This is similar to the standing waves formed on a stretched string. To see how this happens, consider a perfect conductor placed in the yz-plane. A linearly polarized electromagnetic wave moving in the negative x-direction strikes the surface. The electric field cannot have a component parallel to the surface of a perfect...

standing waves in a cavity

Electromagnetic Modes in a Microwave Cavity

Electromagnetic waves can form standing patterns inside a cavity. Household microwaves and lasers are common examples of this effect. When two conducting metal plates are placed parallel at the nodal planes, they create a space where standing waves can exist. The cavity between the plates works like a stretched string fixed at x = 0 and x = L. The distance L must be an integer multiple of half a wavelength. The wavelengths that meet this condition have matching frequencies, and each frequency,...

key terms and concepts

Explore how electromagnetic waves transfer momentum, how reflection changes radiation pressure, and why sunlight shapes star balance and comet tails.

Radiation Pressure in Light and Space | 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.

Pennsylvania State Academic Standards

Earth and Space Science

Earth's Systems

3.3.9-12.H

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-ESS2-4

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.

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Radiation Pressure in Light and Space

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