Cooling flow

Cooling flow

A cooling flow occurs according to the theory that the intracluster medium (ICM) in the centres of galaxy clusters should be rapidly cooling at the rate of tens to thousands of solar masses per year.[1] This should happen as the ICM (a plasma) is quickly losing its energy by the emission of X-rays. The X-ray brightness of the ICM is proportional to the square of its density, which rises steeply towards the centres of many clusters. Also the temperature falls to typically a third or a half of the temperature in the outskirts of the cluster. The typical timescale for the ICM to cool is relatively short, less than a billion years. As material in the centre of the cluster cools out, the pressure of the overlying ICM should cause more material to flow inwards (the cooling flow).

In a steady state, the rate of mass deposition, i.e. the rate at which the plasma cools, is given by

\dot{M} = \frac{2}{5} \frac{L \mu m}{kT},

where L is the bolometric (i.e. over the entire spectrum) luminosity of the cooling region, T is its temperature, k is the Boltzmann constant and μm is the mean molecular mass.

It is currently thought that the very large amounts of expected cooling are in reality much smaller, as there is little evidence for cool X-ray emitting gas in many of these systems[2]. This is the cooling flow problem. Theories for why there is little evidence of cooling include[3]

Heating by AGN is the most popular explanation, as they emit a lot of energy over their lifetimes, and some of the alternatives listed have theoretical problems.


  1. ^ Fabian A.C.: Cooling flows in clusters of galaxies, Annu. Rev. Astron. Astrophys. 1994. 32: 277-318
  2. ^ Peterson J.R., et al.: High-Resolution X-ray Spectroscopic Constrains on Cooling Flow Models for Clusters of Galaxies. ApJ 2003. 590: 207
  3. ^ Peterson J.R., Fabian A.C.: X-ray spectoscopy of cooling clusters, Physics Reports. 2006. 427: 1

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