Radiation pressure is the pressure exerted upon any surface exposed to electromagnetic radiation. The term can also refer to pressures generated by other forms of wave motion, e.g. acoustic radiation pressure. If absorbed, the pressure is the power flux density divided by the speed of light. If the radiation is totally reflected, the radiation pressure is doubled.

For example, the radiation of the Sun at the Earth has a power flux density of 1,368.8485 W/m2, so the radiation pressure is 4.6 µPa (absorbed).

## Discovery

The fact that electromagnetic radiation exerts a pressure upon any surface exposed to it was deduced theoretically by James Clerk Maxwell in 1871 and Adolfo Bartoli in 1876, and proven experimentally by Russian physicist Peter Lebedev in 1900[1] and by Ernest Fox Nichols and Gordon Ferrie Hull in 1901.[2] The pressure is very feeble, but can be detected by allowing the radiation to fall upon a delicately poised vane of reflective metal in a Nichols radiometer (this should not be confused with the Crookes radiometer, whose characteristic motion is not caused by radiation pressure but by impacting gas molecules).

## Theory

### Radiation pressure in classical electromagnetism

According to Maxwell's theory of electromagnetism, an electromagnetic plane wave carries momentum, which can be transferred to a reflecting (or absorbing) surface hit by the wave.

The energy flux (intensity) is expressed by the Poynting vector $\mathbf{S} = \mathbf{E}\times\mathbf{H},$, whose magnitude we denote by S. S divided by the square of the speed of light in free space is the density of the linear momentum of the electromagnetic field. The time-averaged intensity $\langle\mathbf{S}\rangle$ divided by the speed of light in free space is the radiation pressure exerted by an electromagnetic wave on the surface of a target, if the wave is completely absorbed:

$P_{rad}=\frac{\langle S\rangle}{c}$.

This formula is multiplied by a factor of 2, if the wave is actually completely reflected.

### Particle argument

From the perspective of quantum theory, light is made of photons: particles with zero mass at rest but which carry energy and — importantly in this argument — momentum. According to special relativity, because photons are massless their energy (E) and momentum (p) are related by E=pc.[3]

Now consider a beam of light perpendicularly incident on a surface, and let us assume the beam of light is totally absorbed. If we imagine the beam is made of photons, then every second numerous photons strike the surface and are absorbed. The momentum the photons carry is a conserved quantity — that is: it cannot be destroyed — so it must be transferred to the surface; the result is that absorbing the light beam causes the surface to gain momentum.

Newton's second law tells us that force equals rate of change of momentum, so during each second the surface experiences a force (or pressure, as pressure is force per unit area) due to the momentum the photons transfer to it. We have:

Pressure = momentum transferred per second per unit area = energy deposited per second per unit area / c = I/c.

Where I is the intensity of the beam of light (measured in e.g. W/m2).

In the above argument we assumed that the surface totally absorbed the beam, in general light can be transmitted, reflected and/or absorbed. If the light were totally reflected then the radiation pressure is doubled compared to total absorption, this is because the photons arrive with momentum E/c and depart with momentum -E/c (the -ve sign indicates travelling in the opposite direction), so the change of momentum is 2E/c.

### Radiation pressure due to isotropic (e.g. thermal) radiation

It may be shown by electromagnetic theory, by quantum theory, or by thermodynamics, making no assumptions as to the nature of the radiation (other than isotropy), that the pressure against a surface exposed in a space traversed by radiation uniformly in all directions is equal to one third of the total radiant energy per unit volume within that space.[4][5][6][7]

Quantitatively, this can be expressed as [8]

$P_{rad} = \frac{1}{3} u = \frac{1}{3} a T^4$,

for a radiation energy density $u$. The second equality holds if we are considering thermal radiation at a temperature $T$. Here, the radiation constant $a = 4 \sigma / c$, where $\sigma$ is the Stefan-Boltzmann constant, and $c$ is the speed of light.

### In interplanetary space

In astronomy, solar radiation pressure is the force exerted by solar radiation on objects within its reach. Solar radiation pressure is of interest in astrodynamics, as it is one source of the orbital perturbations.

The disturbance force can be expressed simply as:

$F_{SR} = -p_{SR}c_{R}A_{\odot}r_{\oplus\odot}$ [9]

where:

• $F_{SR}$ - Force contributed by the solar radiation pressure.
• $p_{SR}$ - Pressure exerted by the solar radiation.
• $c_{R}$ - Coefficient of reflectivity of the object. $c_{R}=1$ for absolute black body and is generally greater than 1 for other cases. Note: $c_{R}$ should not be confused with albedo or reflection coefficient.
• $A_{\odot}$ - Area of the object exposed to the solar radiation.
• $r_{\oplus\odot}$ - Radial unit vector between object and the Sun.

Radiation pressure is about 10−5 Pa at Earth's distance from the Sun[10] and decreases by the square of the distance from the Sun.

For example, at the boiling point of water (T = 373 K), a blackbody is emitting about 1,080 watts of energy per square meter of surface. This is somewhat below the Sun's 1373 W/m², but still instructive. If the blackbody absorbs 1,080 watts on its Sun-facing surface, it must also emit all 1,080 watts omnidirectionally. The omnidirectional emission is self-cancelling, so that it neither adds nor detracts from the net solar flux force.

By the radiation pressure equation σT4/c; the Sun-facing photon pressure is approximately 0.211 Pa. If the Sun-facing surface is an almost perfect reflector, the force would approach double that (7.22 µPa) depending on how close to an ideal reflector the surface is polished.

While rather small in comparison to chemical thrusters, the radiation pressure force is inexorable and requires no fuel mass. Thus, over months to years, the net (integrated) amount of force is substantial, and is thought to be sufficient to speed interplanetary probes to velocities that could traverse the Earth-Pluto distance in 1/2 to 1/4 the time of a chemically accelerated vessel.

Such feeble pressures are able to produce marked effects upon minute particles like gas ions and electrons, and are important in the theory of electron emission from the Sun, of cometary material, and so on (see also: Yarkovsky effect, YORP effect, Poynting–Robertson effect).

AU distance µPa (µN/m²) N/km² lbf/mi²
0.10 AU = close 915 915 526
0.46 AU = Mercury 43.3 43.3 24.9
0.72 AU = Venus 17.7 17.7 10.2
1.00 AU = Earth 9.15 9.15 5.26
1.52 AU = Mars 3.96 3.96 2.28
5.22 AU = Jupiter 0.34 0.34 0.19

The table shows that the accelerative forces very close to the Sun are very high, and almost of no comparative importance (for macroscopic particles) by the orbital distance of Jupiter. It is for this reason that most interplanetary radiation-pressure probe missions are Sun grazers, whose orbital trajectory passes very close to the Sun so that at midpoint, the probe's reflectors can be turned toward the Sun, adding considerable velocity to the craft.

Because the ratio of surface area to volume (and thus mass) increases with decreasing particle size, dusty (micrometre-size) particles are susceptible to radiation pressure even in the outer solar system. For example, the evolution of the outer rings of Saturn is significantly influenced by radiation pressure.

### In stellar interiors

In stellar interiors the temperatures are very high. Stellar models predict a temperature of 15 MK in the center of the Sun and at the cores of supergiant stars the temperature may exceed 1 GK. As the radiation pressure scales as the fourth power of the temperature, it becomes important at these high temperatures. In the Sun, radiation pressure is still quite small when compared to the gas pressure. In the heaviest non-degenerate stars, radiation pressure is the dominant pressure component.[11]

## Solar sails

Solar sails, a proposed method of spacecraft propulsion, would use radiation pressure from the Sun as a motive force. Private spacecraft Cosmos 1 was to have used this form of propulsion. The idea was proposed as early as 1924 by Soviet scientist Friedrich Zander.

The Japan Aerospace Exploration Agency (JAXA) has successfully unfurled a solar sail in space which has already succeeded in propelling its payload with the IKAROS project.

## Effect on GPS satellites

Variability in solar radiation pressure constitutes the single largest source of error in modelling the orbital dynamics of GPS satellites.[12]

## Radiation pressure in acoustics

In acoustics, radiation pressure is the unidirectional pressure force exerted at an interface between two media due to the passage of a sound wave. If sound is absorbed in the volume during propagation, a body radiation force builds up. In a fluid, this force generates acoustic streaming.

## Radiation stress in surface gravity waves

For surface gravity waves in fluid dynamics, radiation stress is the stress tensor arising from the average excess flux of horizontal momentum – integrated over the water depth – due to the presence of the waves. Variations in radiation stress can give rise to wave-induced streaming (mean currents) especially in the coastal surf zone.

## Laser cooling

Laser cooling is applied to cooling materials very close to absolute zero. Atoms traveling towards a laser light source perceive a doppler effect tuned to the absorption frequency of the target element. The radiation pressure on the atom slows movement in a particular direction until the Doppler effect moves out of the frequency range of the element, causing an overall cooling effect.

## References

1. ^ P. Lebedev, 1901, "Untersuchungen über die Druckkräfte des Lichtes", Annalen der Physik, 1901
2. ^ Nichols, E.F & Hull, G.F. (1903) The Pressure due to Radiation, The Astrophysical Journal,Vol.17 No.5, p.315-351
3. ^ See discussion and references in photon
4. ^ R. Shankar, "Principles of Quantum Mechanics", 2nd edition.
5. ^ Bradley W. Carroll & Dale A. Ostlie, "An Introduction to Modern Astrophysics", 2nd edition.
6. ^ John David Jackson, "Classical Electrodynamics", 1999.
7. ^ Mehran Kardar, "Statistical Physics of Particles".
8. ^ Eric W. Weisstein, "RadiationPressure", MathWorld.
9. ^ David A. Vallado, 2007, "Fundamentals of Astrodynamics and Applications", 3rd ed., Microcosm Press, Hawthorne, California, sec. 8.6.4
10. ^
11. ^ Dale A. Ostlie and Bradley W. Carroll, An Introduction to Modern Astrophysics (2nd edition), page 341, Pearson, San Francisco, CA 2007
12. ^ IPN Progress Report 42-159 (2004)