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• W3098111844 endingPage "577" @default.
• W3098111844 startingPage "567" @default.
• W3098111844 abstract "We study the origin of the non-thermal emission from the intracluster medium, including the excess hard X-ray emission and cluster-wide radio haloes, through fitting two representative models to the Coma cluster. If the synchrotron-emitting relativistic electrons are accelerated in situ from the vast pool of thermal electrons, then a quasi-stationary solution of the kinetic equation with particle acceleration through turbulence at high energies (>200 keV) naturally produces a population of suprathermal electrons responsible for the excess hard X-ray emission through bremsstrahlung. Inverse Compton scattering is negligible at hard X-ray energies in this case. The radio halo flux density constrains the magnetic field strength to a value close to that of equipartition, ∼1 μG. Alternatively, if the relativistic electrons are injected from numerous localized ‘external’ sources, then the hard X-rays are best explained by inverse Compton scattering from GeV electrons, and little of the hard X-radiation has a bremsstrahlung origin. In this case, the magnetic field strength is constrained to ∼0.1–0.2 μG. Both models assume that the non-thermal emissions are generated by a single electron spectrum, so that only two free parameters, well constrained by the observed hard X-ray and radio halo spectra, are needed in either case. Measurements of the cluster magnetic field will distinguish between the models." @default.
• W3098111844 created "2020-11-23" @default.
• W3098111844 creator A5002771039 @default.
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• W3098111844 date "2002-09-01" @default.
• W3098111844 modified "2023-10-06" @default.
• W3098111844 title "The origin of radio haloes and non-thermal emission in clusters of galaxies" @default.
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• W3098111844 doi "https://doi.org/10.1046/j.1365-8711.2002.05937.x" @default.
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