Cluster Mergers and Non-Thermal Phenomena: A Statistical Magneto-Turbulent Model

By R. Cassano, Gianfranco Brunetti. 2004

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With the aim to investigate the statistical properties and the connection between thermal and non-thermal properties of the ICM in galaxy clusters, we have developed a statistical magneto-turbulent model which describes, at the same time, the evolution of the thermal and non-thermal emission from galaxy clusters. In particular, starting from the cosmological evolution of clusters, we follow cluster. mergers, calculate the spectrum of the magnetosonic waves generated in the ICM during these mergers, the evolution of relativistic electrons and the resulting synchrotron and Inverse Compton spectra. We show that the broad band (radio and hard x-ray) non-thermal spectral properties of galaxy clusters can be well accounted for by our model for viable values of the parameters (here we adopt a EdS cosmology).

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/670721cdf115aa56c90b01edfc66641c25cf28dc

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Citations in the corpus

Compressible turbulence in galaxy clusters: physics and stochastic particle re-acceleration (2007, background): “…interactions via gyroresonance and the Transit-Time Damping (TTD) (Chandran 2000; Yan & Lazarian 2002, 2004; Farmer & Goldreich 2004; Cassano & Brunetti 2005) as well as the non-resonance acceleration of cosmic rays by large scale compressible motions (see Ptuskin 1988, Chandran…”
Turbulent gas motions in galaxy cluster simulations: the role of smoothed particle hydrodynamics viscosity (2005, methodology): “Following Cassano & Brunetti (2005), the spectrum of the magnetic fluctuations associated with Fast Modes is computed under stationary conditions taking into account the damping rate of these modes with thermal electrons,Γk = Γok.”
Massive and refined - II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution (2010, methodology): “The combination of these points implies that the energy of turbulence should scale with the cluster thermal energy, E t urb ∼ A · E th ∼ M 3 / 2 vir (where A 1, e.g. Cassano & Brunetti 2005).”
GMRT radio halo survey in galaxy clusters at z = 0.2–0.4 - II. The eBCS clusters and analysis of the complete sample (2008, background): “Expectations were made for the occurrence of giant1 radio halos as a function of redshift and mass (Cassano & Brunetti 2005, hereinafter CB05; Cassano, Brunetti & Setti 2006, hereinafter CBS06; Cassano et al. 2008).”
Evolving turbulence and magnetic fields in galaxy clusters (2005, background): “The turbulent flow of magnetized gas can accelerate relativistic particles required to produce cluster radio haloes (Tribble 1993b; Brunetti et al. 2004; Cassano & Brunetti 2005).”
Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio haloes to gamma-rays (2010, methodology): “…a ”sonic” turbulent–forcing, Ioτcl ≈ ǫth, where τcl ∼ 3− 6 Gyrs is the life–time of massive clusters, and a typical merging history of massive clusters (eg., Cassano & Brunetti 2005 and ref. therein), we expect ǫCR ≤ few percent of the thermal energy density, provided that relativistic protons…”