Radiation pressure | Wikipedia audio article
Channel: wikipedia tts
Date: 2019-06-23

This is an audio version of the Wikipedia Article:
https://en.wikipedia.org/wiki/Radiation_pressure


00:02:28 1 Discovery
00:05:08 2 Theory
00:05:41 2.1 Radiation pressure from momentum of an electromagnetic wave
00:09:13 2.2 Radiation pressure from reflection
00:11:18 2.3 Radiation pressure by emission
00:12:58 2.4 Radiation pressure in terms of photons
00:15:24 2.5 Compression in a uniform radiation field
00:17:32 3 Solar radiation pressure
00:18:52 3.1 Pressures of absorption and reflection
00:23:56 3.2 Radiation pressure perturbations
00:29:15 3.3 Solar sails
00:30:21 4 Cosmic effects of radiation pressure
00:30:48 4.1 The early universe
00:31:10 4.2 Galaxy formation and evolution
00:31:54 4.3 Clouds of dust and gases
00:32:34 4.4 Clusters of stars
00:33:33 4.5 Star formation
00:34:23 4.6 Stellar planetary systems
00:35:21 4.7 Stellar interiors
00:36:09 4.8 Comets
00:36:47 5 Laser applications of radiation pressure
00:36:59 5.1 Optical tweezers
00:41:06 5.2 Other examples



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SUMMARY
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Radiation pressure is the pressure exerted upon any surface due to the exchange of momentum between the object and the electromagnetic field. This includes the momentum of light or electromagnetic radiation of any wavelength which is absorbed, reflected, or otherwise emitted (e.g. black-body radiation) by matter on any scale (from macroscopic objects to dust particles to gas molecules).The forces generated by radiation pressure are generally too small to be noticed under everyday circumstances; however, they are important in some physical processes. This particularly includes objects in outer space where it is usually the main force acting on objects besides gravity, and where the net effect of a tiny force may have a large cumulative effect over long periods of time. For example, had the effects of the sun's radiation pressure on the spacecraft of the Viking program been ignored, the spacecraft would have missed Mars orbit by about 15,000 km (9,300 mi). Radiation pressure from starlight is crucial in a number of astrophysical processes as well. The significance of radiation pressure increases rapidly at extremely high temperatures, and can sometimes dwarf the usual gas pressure, for instance in stellar interiors and thermonuclear weapons.
Radiation pressure can equally well be accounted for by considering the momentum of a classical electromagnetic field or in terms of the momenta of photons, particles of light. The interaction of electromagnetic waves or photons with matter may involve an exchange of momentum. Due to the law of conservation of momentum, any change in the total momentum of the waves or photons must involve an equal and opposite change in the momentum of the matter it interacted with (Newton's third law of motion), as is illustrated in the accompanying figure for the case of light being perfectly reflected by a surface. This transfer of momentum is the general explanation for what we term radiation pressure.