Cosmic rays and thermal instability in self-regulating cooling flows of massive galaxy clusters

Open Access

Fig. 2.

Ratio of the cooling time to the free-fall time for the initial conditions of the cluster for various values of the core radius r_core assuming an BH with a mass of M_BH = 1.6 × 10¹⁰ M_⊙. Without the mass of the BH, the initial cluster profile dips lower in the centre for the chosen core radius of 13 kpc (red line).

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