Particle reacceleration in Coma cluster: radio properties and hard X-ray emission

Details Particle reacceleration in Coma cluster: radio properties and hard X-ray emission Particle reacceleration in Coma cluster: radio properties and hard X-ray emission

2000-08-31

arxiv.org/abs/astro-ph/0008518v1

Mon.Not.Roy.Astron.Soc. 320 (2001) 365

Astronomy and Astrophysics

Astrophysics

15 pages, 13 figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2001.03978.x

The radio spectral index map of the Coma halo shows a progressive steepening of the spectral index with increasing radius. Such a steepening cannot be simply justified by models involving continuous injection of fresh particles in the Coma halo or by models involving diffusion of fresh electrons from the central regions. We propose a {\it two phase} model in which the relativistic electrons injected in the Coma cluster by some processes (starbursts, AGNs, shocks, turbulence) during a {\it first phase} in the past are systematically reaccelerated during a {\it second phase} for a relatively long time ($\sim$ 1 Gyr) up to the present time. We show that for reacceleration time scales of $\sim 0.1$ Gyr this hypothesis can well account for the radio properties of Coma C. For the same range of parameters which explain Coma C we have calculated the expected fluxes from the inverse Compton scattering of the CMB photons finding that the hard X-ray tail discovered by BeppoSAX may be accounted for by the stronger reacceleration allowed by the model. The possibility of extending the main model assumptions and findings to the case of the other radio haloes is also discussed, the basic predictions being consistent with the observations.

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