Abstract
We show that the magnetic field may become very important in the inner regions of cluster cooling flows. The magnetic pressure becomes comparable to the thermal pressure within a radius of typically 1 – 10 kpc. Within this region, reconnection of the magnetic field becomes efficient and magnetic energy is released at a rate of 1041 – 1043 erg s-1. Buoyancy is ineffective in transporting the magnetic field out of the cooling flow.
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© 1988 Kluwer Academic Publishers
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Soker, N., Sarazin, C.L. (1988). The Role of Magnetic Fields in Cluster Cooling Flows. In: Fabian, A.C. (eds) Cooling Flows in Clusters and Galaxies. NATO ASI Series, vol 229. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-2953-1_47
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DOI: https://doi.org/10.1007/978-94-009-2953-1_47
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-7828-3
Online ISBN: 978-94-009-2953-1
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