The role of thermal conductivity in the evolution of the gas in clusters of galaxies

Details The role of thermal conductivity in the evolution of the gas in clusters of galaxies The role of thermal conductivity in the evolution of the gas in clusters of galaxies

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...164....6f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 164, no. 1, Aug. 1986, p. 6-16.

Astronomy and Astrophysics

Astrophysics

23

Cooling Flows (Astrophysics), Cosmic Gases, Galactic Clusters, Galactic Evolution, Gas Temperature, Intergalactic Media, Thermal Conductivity, Astronomical Models, Bremsstrahlung, Brightness Distribution, X Ray Astronomy

Scientific paper

The evolution of the gas in rich regular clusters of galaxies without central dominant galaxies is investigated using hydrodynamical modeling. All models exhibit central cooling, which leads in some cases to collapse of the gas core before the present epoch. A massive galaxy may then be formed at the expense of the resulting cooling flow. On the other hand, a massive galaxy initially present at the cluster core will favor the collapse. Thus, it is expected that collapsed clusters are more likely to have central dominant galaxies. Analysis of data from 12 Abell clusters gives moderate support for this scenario. It is verified that thermal conductivity, which is expected to occur at a fraction (eta) of the Spitzer value owing to the inhibiting effects of the intracluster magnetic field, is of great importance in determining the structure of the gas and the collapse epoch. The cool X-ray clusters observed by Perrenod and Henry (1981) at about z = 0.4 are probably postcollapse clusters, which then requires eta greater than about 0.003, whereas eta less than about 0.0003 accounts for the absence of central cooling in Coma-like clusters. It is suggested that the cluster A576 is just beginning to collapse.

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