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Date and Time of the Query: 2019-04-24 T07:14:22 PDT
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For refcode 2008A&A...486L..31C:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2008A&A...486L..31C A morphological comparison between giant radio halos and radio mini-halos in galaxy clusters Cassano, R.; Gitti, M.; Brunetti, G. Abstract. In this letter we present a morphological comparison between giant radio halos and radio mini-halos in galaxy clusters based on radio-X-ray luminosity, P_1.4_-L_X, and radio luminosity-size, P_1.4_-R_H, correlations. We report evidence that P_1.4_-L_X_ and P_1.4_-R_H_ trends may also exist for mini-halos: mini-halo clusters share the same region of giant halo clusters in the (P_1.4_,L_X) plane, whereas they are clearly separated in the (P_1.4_,R_H) plane. The synchrotron emissivity of mini-halos is found to be more than 50 times larger than that of giant halos, implying a very efficient process for their origins. By assuming a scenario of sporadical turbulent particle re-acceleration for both giant and mini halos, we discuss basic physical differences between these sources. Regardless of the origin of the turbulence, a more efficient source of injection of particles, which eventually takes part in the re-acceleration process, is required in mini-halos, and this may result from the central radio galaxy or from proton-proton collisions in the dense cool core regions. Key words: radiation mechanism: non-thermal, galaxies: clusters: general, radio continuum: general, X-rays: general
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