Galaxy cluster merger shocks are the likely source of relativistic electrons, but many observations do not fit into the standard acceleration models. In particular, there is a long-standing discrepancy between the radio derived Mach numbers M radio and the Mach numbers derived from X-ray measurements, M X . Here, we show how superdiffusive electron transport and superdiffusive shock acceleration (SSA) can help to solve this problem. We present a heuristic derivation of the superlinear time growth of the mean square displacement of particles, 〈Δx 2 〉∝ t β , and of the particle energy spectral index in the framework of SSA. The resulting expression for the radio spectral index a is then used to determine the superdiffusive exponent β from the observed values of α and of the compression ratio for a number of radio relics. Therefore, the fact that M radio > M X can be explained by SSA without the need to make assumptions on the energy spectrum of the seed electrons to be re-accelerated. We also consider the acceleration times obtained in the diffusive case, based both on the Bohm diffusion coefficient and on the quasi-linear diffusion coefficient. While in the latter case the acceleration time is consistent with the estimated electron energy loss time, in the former case it is much shorter.
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|Titolo:||Understanding the radio spectral indices of galaxy cluster relics by superdiffusive shock acceleration|
ZIMBARDO, Gaetano [Formal Analysis] (Corresponding)
PERRI, SILVIA [Formal Analysis]
|Data di pubblicazione:||2018|
|Appare nelle tipologie:||1.1 Articolo in rivista|