Synchrotron Radiation - NASA

Synchrotron RadiationThe Synchrotron Radiation , the emission of very relativistic and ultrarelativisticelectrons gyrating in a magnetic field, is the process which dominates much of highenergy astrophysics. It was originally observed in early betatron experiments inwhich electrons were first accelerated to ultrarelativistic energies. This process isresponsible for the radio emission from the Galaxy, from supernova remnants andextragalactic radio sources. It is also responsible for the non-thermal optical andX-ray emission observed in the Crab Nebula and possibly for the optical and X-raycontinuum emission of wordnon-thermalis used frequently in high energy astrophysics to describe theemission of high energy particles .

Particles of a particular energy E, or Lorentz factor γ, are often expected to have an isotropic distribution of pitch angles and therefore we can work out their average energy loss rate by averaging over such a distribution of pitch angles p(θ)dθ = 1

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