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Klein–Nishina distribution of scattering-angle cross sections over a range of commonly encountered energies. Electron-photon scattering cross section In particle physics , the Klein–Nishina formula gives the differential cross section (i.e. the "likelihood" and angular distribution) of photons scattered from a single free electron ...
The differential angular range of the scattered particle at angle θ is the solid angle element dΩ = sin θ dθ dφ. The differential cross section is the quotient of these quantities, dσ / dΩ . It is a function of the scattering angle (and therefore also the impact parameter), plus other observables such as the momentum of the ...
The collision causes the photon wavelength to increase by somewhere between 0 (for a scattering angle of 0°) and twice the Compton wavelength (for a scattering angle of 180°). [32] Thomson scattering is the classical elastic quantitative interpretation of the scattering process, [26] and this can be seen to happen with lower, mid-energy, photons.
Fig. 1: Schematic diagram of Compton's experiment. Compton scattering occurs in the graphite target on the left. The slit passes X-ray photons scattered at the selected angle and their average energy rate is measured using Bragg scattering from the crystal on the right in conjunction with an ionization chamber.
where and ′ are the angles between and ′ and some direction ″. This condition puts a constraint on the allowed form for f ( θ ) {\displaystyle f(\theta )} , i.e., the real and imaginary part of the scattering amplitude are not independent in this case.
In gamma-ray spectrometry, the Compton edge is a feature of the measured gamma-ray energy spectrum that results from Compton scattering in the detector material. It corresponds to the highest energy that can be transferred to a weakly bound electron of a detector's atom by an incident photon in a single scattering process, and manifests itself as a ridge in the measured gamma-ray energy spectrum.
A Lambertian scatterer will then scatter this light according to the same cosine law as a Lambertian emitter. This means that although the radiance of the surface depends on the angle from the normal to the illuminating source, it will not depend on the angle from the normal to the observer.
The probability of finding | ′ is found by evaluating | ′ |.. In case of constant perturbation, ′ is calculated by