Physics:Synchrotron radiation

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Short description: Electromagnetic radiation emitted by charged particles accelerated perpendicular to their velocity


Synchrotron radiation (also known as magnetobremsstrahlung radiation) is the electromagnetic radiation emitted when relativistically charged particles are subject to an acceleration perpendicular to their velocity (a ⊥ v). It is produced artificially in some types of particle accelerators or naturally by fast electrons moving through magnetic fields. The radiation produced in this way has a characteristic polarization, and the frequencies generated can range over a large portion of the electromagnetic spectrum.[1]

Pictorial representation of the radiation emission process by a source moving around a Schwarzschild black hole in a de Sitter universe.

Synchrotron radiation is similar to bremsstrahlung radiation, which is emitted by a charged particle when the acceleration is parallel to the direction of motion. The general term for radiation emitted by particles in a magnetic field is gyromagnetic radiation, for which synchrotron radiation is the ultra-relativistic special case. Radiation emitted by charged particles moving non-relativistically in a magnetic field is called cyclotron emission.[2] For particles in the mildly relativistic range (≈85% of the speed of light), the emission is termed gyro-synchrotron radiation.[3]

In astrophysics, synchrotron emission occurs, for instance, due to ultra-relativistic motion of a charged particle around a black hole.[4] When the source follows a circular geodesic around the black hole, the synchrotron radiation occurs for orbits close to the photosphere where the motion is in the ultra-relativistic regime.

Synchrotron radiation from a bending magnet
Synchrotron radiation from an undulator
Synchrotron radiation from an astronomical source

History

Synchrotron radiation was first observed by technician Floyd Haber, on April 24, 1947, at the 70 MeV electron synchrotron of the General Electric research laboratory in Schenectady, New York.[5] While this was not the first synchrotron built, it was the first with a transparent vacuum tube, allowing the radiation to be directly observed.[6]

As recounted by Herbert Pollock:[7]

On April 24, Langmuir and I were running the machine and as usual were trying to push the electron gun and its associated pulse transformer to the limit. Some intermittent sparking had occurred and we asked the technician to observe with a mirror around the protective concrete wall. He immediately signaled to turn off the synchrotron as "he saw an arc in the tube". The vacuum was still excellent, so Langmuir and I came to the end of the wall and observed. At first we thought it might be due to Cherenkov radiation, but it soon became clearer that we were seeing Ivanenko and Pomeranchuk radiation.[8]

Description

A direct consequence of Maxwell's equations is that accelerated charged particles always emit electromagnetic radiation. Synchrotron radiation is the special case of charged particles moving at relativistic speed undergoing acceleration perpendicular to their direction of motion, typically in a magnetic field. In such a field, the force due to the field is always perpendicular to both the direction of motion and to the direction of field, as shown by the Lorentz force law.

The power carried by the radiation is found (in SI units) by the relativistic Larmor formula:[9][10]

[math]\displaystyle{ P_\gamma = \frac{q^2}{6 \pi \varepsilon_0 c^3} a^2 \gamma^4 = \frac{q^2 c}{6 \pi \varepsilon_0} \frac{\beta^4 \gamma^4}{\rho^2} , }[/math] where

  • [math]\displaystyle{ \varepsilon_0 }[/math] is the vacuum permittivity,
  • [math]\displaystyle{ q }[/math] is the particle charge,
  • [math]\displaystyle{ a }[/math] is the magnitude of the acceleration,
  • [math]\displaystyle{ c }[/math] is the speed of light,
  • [math]\displaystyle{ \gamma }[/math] is the Lorentz factor,
  • [math]\displaystyle{ \beta = v/c }[/math],
  • [math]\displaystyle{ \rho }[/math] is the radius of curvature of the particle trajectory.

The force on the emitting electron is given by the Abraham–Lorentz–Dirac force.

When the radiation is emitted by a particle moving in a plane, the radiation is linearly polarized when observed in that plane, and circularly polarized when observed at a small angle. Considering quantum mechanics, however, this radiation is emitted in discrete packets of photons and has significant effects in accelerators called quantum excitation. For a given acceleration, the average energy of emitted photons is proportional to [math]\displaystyle{ \gamma^3 }[/math] and the emission rate to [math]\displaystyle{ \gamma }[/math].

From accelerators

Main page: Engineering:Synchrotron light source

Circular accelerators will always produce gyromagnetic radiation as the particles are deflected in the magnetic field. However, the quantity and properties of the radiation are highly dependent on the nature of the acceleration taking place. For example, due to the difference in mass, the factor of [math]\displaystyle{ \gamma^4 }[/math] in the formula for the emitted power means that electrons radiate energy at approximately 1013 times the rate of protons.[11]

Energy loss from synchrotron radiation in circular accelerators was originally considered a nuisance, as additional energy must be supplied to the beam in order to offset the losses. However, beginning in the 1980s, circular electron accelerators known as light sources have been constructed to deliberately produce intense beams of synchrotron radiation for research.[12]

In astronomy

Messier 87's astrophysical jet, HST image. The blue light from the jet emerging from the bright AGN core, towards the lower right, is due to synchrotron radiation.

Synchrotron radiation is also generated by astronomical objects, typically where relativistic electrons spiral (and hence change velocity) through magnetic fields. Two of its characteristics include power-law energy spectra and polarization.[13] It is considered to be one of the most powerful tools in the study of extra-solar magnetic fields wherever relativistic charged particles are present. Most known cosmic radio sources emit synchrotron radiation. It is often used to estimate the strength of large cosmic magnetic fields as well as analyze the contents of the interstellar and intergalactic media.[14]

History of detection

This type of radiation was first detected in a jet emitted by Messier 87 in 1956 by Geoffrey R. Burbidge,[15] who saw it as confirmation of a prediction by Iosif S. Shklovsky in 1953. However, it had been predicted earlier (1950) by Hannes Alfvén and Nicolai Herlofson.[16] Solar flares accelerate particles that emit in this way, as suggested by R. Giovanelli in 1948 and described by J.H. Piddington in 1952.[17]

T. K. Breus noted that questions of priority on the history of astrophysical synchrotron radiation are complicated, writing:

Crab Nebula. The bluish glow from the central region of the nebula is due to synchrotron radiation.

From supermassive black holes

It has been suggested that supermassive black holes produce synchrotron radiation in "jets", generated by the gravitational acceleration of ions in their polar magnetic fields. The nearest such observed jet is from the core of the galaxy Messier 87. This jet is interesting for producing the illusion of superluminal motion as observed from the frame of Earth. This phenomenon is caused because the jets are travelling very near the speed of light and at a very small angle towards the observer. Because at every point of their path the high-velocity jets are emitting light, the light they emit does not approach the observer much more quickly than the jet itself. Light emitted over hundreds of years of travel thus arrives at the observer over a much smaller time period, giving the illusion of faster than light travel, despite the fact that there is actually no violation of special relativity.[18]

Pulsar wind nebulae

A class of astronomical sources where synchrotron emission is important is pulsar wind nebulae, also known as plerions, of which the Crab nebula and its associated pulsar are archetypal. Pulsed emission gamma-ray radiation from the Crab has recently been observed up to ≥25 GeV,[19] probably due to synchrotron emission by electrons trapped in the strong magnetic field around the pulsar. Polarization in the Crab nebula[20] at energies from 0.1 to 1.0 MeV, illustrates this typical property of synchrotron radiation.

Interstellar and intergalactic media

Much of what is known about the magnetic environment of the interstellar medium and intergalactic medium is derived from observations of synchrotron radiation. Cosmic ray electrons moving through the medium interact with relativistic plasma and emit synchrotron radiation which is detected on Earth. The properties of the radiation allow astronomers to make inferences about the magnetic field strength and orientation in these regions. However, accurate calculations of field strength cannot be made without knowing the relativistic electron density.[14]

In supernovae

When a star explodes in a supernova, the fastest ejecta move at semi-relativistic speeds approximately 10% the speed of light.[21] This blast wave gyrates electrons in ambient magnetic fields and generates synchrotron emission, revealing the radius of the blast wave at the location of the emission.[22] Synchrotron emission can also reveal the strength of the magnetic field at the front of the shock wave, as well as the circumstellar density it encounters, but strongly depends on the choice of energy partition between the magnetic field, proton kinetic energy, and electron kinetic energy. Radio synchrotron emission has allowed astronomers to shed light on mass loss and stellar winds that occur just prior to stellar death.[23][24]

See also

Notes

  1. ↑ "What is synchrotron radiation?" (in en). NIST. 2010-03-02. https://www.nist.gov/pml/sensor-science/what-synchrotron-radiation. 
  2. ↑ Monreal, Benjamin (Jan 2016). "Single-electron cyclotron radiation". Physics Today 69 (1): 70. doi:10.1063/pt.3.3060. Bibcode: 2016PhT....69a..70M. 
  3. ↑ Chen, Bin. "Radiative processes from energetic particles II: Gyromagnetic radiation". https://web.njit.edu/~binchen/phys780/LectureNotes/lec21.pdf. 
  4. ↑ Brito, João P. B.; Bernar, Rafael P.; Crispino, Luís C. B. (11 June 2020). "Synchrotron geodesic radiation in Schwarzschild–de Sitter spacetime" (in en). Physical Review D 101 (12): 124019. doi:10.1103/PhysRevD.101.124019. ISSN 2470-0010. Bibcode: 2020PhRvD.101l4019B. 
  5. ↑ Elder, F. R.; Gurewitsch, A. M.; Langmuir, R. V.; Pollock, H. C. (1 June 1947). "Radiation from Electrons in a Synchrotron". Physical Review (American Physical Society) 71 (11): 829–830. doi:10.1103/physrev.71.829.5. ISSN 0031-899X. Bibcode: 1947PhRv...71..829E. 
  6. ↑ Mitchell, Edward; Kuhn, Peter; Garman, Elspeth (May 1999). "Demystifying the synchrotron trip: a first time user's guide". Structure 7 (5): R111–R121. doi:10.1016/s0969-2126(99)80063-x. PMID 10378266. 
  7. ↑ Pollock, Herbert C. (March 1983). "The discovery of synchrotron radiation". American Journal of Physics 51 (3): 278–280. doi:10.1119/1.13289. Bibcode: 1983AmJPh..51..278P. 
  8. ↑ Iwanenko, D.; Pomeranchuk, I. (1 June 1944). "On the Maximal Energy Attainable in a Betatron". Physical Review (American Physical Society) 65 (11–12): 343. doi:10.1103/physrev.65.343. ISSN 0031-899X. Bibcode: 1944PhRv...65..343I. 
  9. ↑ Wilson, E. J. N. (2001). An introduction to particle accelerators. Oxford: Oxford University Press. pp. 221–223. ISBN 0-19-850829-8. 
  10. ↑ Fitzpatrick, Richard (in en). Classical Electromagnetism. p. 299. https://farside.ph.utexas.edu/teaching/jk1/Electromagnetism.pdf. 
  11. ↑ Conte, Mario; MacKay, William (2008). An introduction to the physics of particle accelerators (2nd ed.). Hackensack, N.J.: World Scientific. p. 166. ISBN 978-981-277-960-1. 
  12. ↑ "History: Of X-rays and synchrotrons". 21 September 2017. https://lightsources.org/history/. 
  13. ↑ Vladimir A. Bordovitsyn, "Synchrotron Radiation in Astrophysics" (1999) Synchrotron Radiation Theory and Its Development, ISBN:981-02-3156-3
  14. ↑ 14.0 14.1 Klein, Ulrich (2014). Galactic and intergalactic magnetic fields. Cham, Switzerland & New York: Springer. ISBN 978-3-319-08942-3. OCLC 894893367. 
  15. ↑ Burbidge, G. R. (1956). "On Synchrotron Radiation from Messier 87". The Astrophysical Journal (IOP Publishing) 124: 416. doi:10.1086/146237. ISSN 0004-637X. Bibcode: 1956ApJ...124..416B. 
  16. ↑ Alfvén, H.; Herlofson, N. (1 June 1950). "Cosmic Radiation and Radio Stars". Physical Review (APS) 78 (5): 616. doi:10.1103/physrev.78.616. ISSN 0031-899X. Bibcode: 1950PhRv...78..616A. 
  17. ↑ Piddington, J. H. (1953). "Thermal Theories of the High-Intensity Components of Solar Radio-Frequency Radiation". Proceedings of the Physical Society. Section B (IOP Publishing) 66 (2): 97–104. doi:10.1088/0370-1301/66/2/305. ISSN 0370-1301. Bibcode: 1953PPSB...66...97P. 
  18. ↑ Chase, Scott I.. "Apparent Superluminal Velocity of Galaxies". http://math.ucr.edu/home/baez/physics/Relativity/SpeedOfLight/Superluminal/superluminal.html. 
  19. ↑ Aliu, E.; Anderhub, H.; Antonelli, L. A.; Antoranz, P.; Backes, M. et al. (21 November 2008). "Observation of Pulsed γ-Rays Above 25 GeV from the Crab Pulsar with MAGIC". Science 322 (5905): 1221–1224. doi:10.1126/science.1164718. ISSN 0036-8075. PMID 18927358. Bibcode: 2008Sci...322.1221A. 
  20. ↑ Dean, A. J.; Clark, D. J.; Stephen, J. B.; McBride, V. A.; Bassani, L. et al. (29 August 2008). "Polarized Gamma-Ray Emission from the Crab". Science (American Association for the Advancement of Science (AAAS)) 321 (5893): 1183–1185. doi:10.1126/science.1149056. ISSN 0036-8075. PMID 18755970. Bibcode: 2008Sci...321.1183D. 
  21. ↑ Soderberg, A.; Chevalier, R. A.; Kulkarni, S. R.; Frail, D. A. (November 2006). "The Radio and X-Ray Luminous SN 2003bg and the Circumstellar Density Variations around Radio Supernovae". The Astrophysical Journal 651 (2): 1005–1018. doi:10.1086/507571. 
  22. ↑ Chevalier, R. A. (May 1998). "Synchrotron Self-Absorption in Radio Supernovae". The Astrophysical Journal 499 (2): 810–819. doi:10.1086/305676. 
  23. ↑ Margutti, Raffaella et al. (February 2017). "Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C". The Astrophysical Journal 835 (2): 140. doi:10.3847/1538-4357/835/2/140. 
  24. ↑ DeMarchi, Lindsay et al. (October 2022). "Radio Analysis of SN2004C Reveals an Unusual CSM Density Profile as a Harbinger of Core Collapse". The Astrophysical Journal 938 (1): 84. doi:10.3847/1538-4357/ac8c26. 

References

External links



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