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.

Since (dE/dt) is a Lorentz invariant, we recover the formula (8). Recalling that c2 = (µ0ε0)−1, let us rewrite this in the following way − dE dt = 2 e4 6πε2 0c4m2e! v c 2 c B2 2µ0 γ2 sin2 θ (12) The quantity in the first set of round brackets on the right-hand side of (8) is the Thomson cross-section σT. Therefore − dE dt ...

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