Thomsonszóródásnak

Thomsonszóródásnak, more commonly known as Thomson scattering, is a physical phenomenon observed when electromagnetic radiation, such as light, interacts with free electrons. This scattering process is elastic, meaning the photons do not lose energy in the interaction. The incident photon is absorbed by an electron, which then re-emits a photon of the same energy and wavelength in a different direction. The key characteristic of Thomson scattering is that the wavelength of the scattered radiation remains unchanged.

This effect is named after J.J. Thomson, who developed the classical theory to explain it in 1906. His model treated the electron as a charged sphere that oscillates when exposed to the oscillating electric field of an electromagnetic wave. This oscillation then causes the electron to re-radiate the electromagnetic wave. While Thomson's classical model provides a good approximation for many scenarios, a more complete description requires quantum electrodynamics.

Thomson scattering is a significant process in various astrophysical contexts. For instance, it plays a crucial role in the interstellar medium and in the atmospheres of stars. The Sun's corona, a region of hot, ionized gas, exhibits Thomson scattering, which is responsible for the faint, continuous spectrum observed from it. Understanding Thomson scattering is essential for interpreting astronomical observations and for modeling the behavior of plasmas in space. The intensity and polarization of the scattered light depend on the properties of the electron plasma and the incident radiation.