High-resolution simulation of magnetic fields in galaxy clusters

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Project objective

The interaction between magnetic fields and hot intra-cluster medium is a key open question concerning galaxy clusters in cosmology. Magnetic fields are thought to operate in the cooling flow paradox (the theoretically expected cooling rate of the intra-cluster medium is orders of magnitudes larger than the one observed) , in cold fronts ( the sharp observed X-ray features suggest suppression of thermal conductivity) and in the missing mass problem (the mass estimated from X-ray data using hydrostatic equilibrium is often lower than that inferred from the dynamics of member galaxies or from gravitational lensing) . The goal of this project is to extend previous numerical work - which gave the first consistent picture of how magnetic fields evolve in galaxy clusters - towards more realistic simulations, using higher resolution and including radiative cooling processes . The ability to describe regimes where magnetic fields dominate cluster dynamics is needed, as observations indicate strong magnetic fields within clusters ' cooling flow regions. This project would lead to the first 3D MHD simulations of galaxy clusters with radiative cooling, and is expected to have substantial impact on the scientific discussion about discrepancies between theoretical predictions and observations of cooling flows in galaxy clusters. The simulations would also shed new light on other open questions related to magnetic fields in galaxy clusters.

Original text from CORDIS.

Participants

• UNIVERSITA DEGLI STUDI DI PADOVA · PADOVACoordinatorItaly

Links

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