Astrophysics (Index)About

synchrotron radiation

(magneto-brems, magneto-bremsstrahlung, magnetobremsstrahlung, MBS)
(radiation emitted when high-speed charged particles are accelerated)

Synchrotron radiation (or magnetobremsstrahlung, magneto-bremsstrahlung, magneto-brems, MBS) is radiation emitted by a charged particle traveling at near the speed of light when it is accelerated. It was first observed in a synchrotron (particle accelerator). Nature can generate it in space within magnetic fields. Characteristics:

Radiation from slower-moving charged particles is termed cyclotron radiation.

Since synchrotron radiation is (at least somewhat) directional, thus sometimes not aimed at us, often it con only be inferred by its effects, e.g., clouds that scatter it or are warmed and produce black body radiation. The synchrotron luminosity of directly-observed synchrotron radiation can be worked out by the spectrum, looking for the power law "shape", but when indirectly observed, more modeling is required to work it out.

Proton synchrotron radiation is that specifically generated by protons to distinguish it from the more frequent electron-generated radiation. It is found in proton accelerators and in astrophysical phenomena that accelerate protons to relativistic speeds. It is less common because a proton's much larger mass makes achieving the relativistic speeds less common.

A contributor to the spectrum of observed synchrotron radiation is synchrotron self-absorption and synchrotron self-scattering. The latter refers to absorption and subsequent emission, and a synchrotron-specific radiative transfer, with photons generated, then absorbed/re-emitted before leaving the medium. Of the synchrotron spectrum the lower-frequency (longer-wavelength) photons are more likely to be absorbed, thus the net effect on the spectrum seen externally is a reduction at the low-frequency end.


(physics,EMR,magnetism)
Further reading:
http://en.wikipedia.org/wiki/Synchrotron_radiation
http://www-astro.physics.ox.ac.uk/~garret/teaching/lecture5-2011.pdf

Referenced by pages:
continuum emission
curvature radiation
cyclotron radiation
electron scattering
FRB121102
magnetic field
maser
microwave
polarization
power law
pulsar wind nebula (PWN)
radio relics
radio galaxy (RG)
spectral index (α)
spectral signature
synchrotron self-Compton (SSC)
standard model of a flare

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