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Cosmic magnetism evolution using cosmological simulations

Published online by Cambridge University Press:  29 March 2021

Stela Adduci Faria Open the ORCID record for Stela Adduci Faria [Opens in a new window] ,
Elisabete M. de Gouveia Dal Pino  and
Paramita Barai Open the ORCID record for Paramita Barai [Opens in a new window]
Stela Adduci Faria
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, University of São Paulo (USP), São Paulo, Brazil e-mail: [email protected]
Elisabete M. de Gouveia Dal Pino
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, University of São Paulo (USP), São Paulo, Brazil e-mail: [email protected]
Paramita Barai
Affiliation:
Núcleo de Astrofísica - Universidade Cruzeiro do Sul (NAT - UNICSUL), São Paulo, Brazil
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Abstract

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The Intergalactic Medium (IGM) is the region comprising the environment between the galaxies. Gamma-ray observations have provided lower limits to IGM magnetic fields of the order of ≳10–16 G. Magnetic fields are continuously ejected from galaxies by jets and galactic winds. However, the origin and evolution of cosmic magnetic fields in the more diffuse regions, like voids, is still debated. The difficulties in directly measuring magnetic fields and their coherent scales, make hydrodynamic and magnetohydrodynamic (MHD) cosmological simulations useful tools to shed light on this debate. As a first approach, we have performed hydrodynamic cosmological simulations assuming energy equipartition as an initial condition between the baryonic gas and the magnetic field, starting at z = 8, to track the evolution of magnetic fields, and compare with results of MHD simulations. We have found that for halos and cores, our results are comparable to the MHD description. For the less dense regions, the equipartition condition clearly overestimates the observed limits. In forthcoming work, we will investigate MHD simulations of cosmological evolution and amplification of seed magnetic fields, considering all relevant feedback processes and exploring turbulent dynamo amplification versus primordial mechanisms across cosmological timescales.

Keywords

Magneto-hydrodynamicsCosmic Ray PropagationCosmological hydrodynamical simulationsOrigin of magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S359: Galaxy Evolution and Feedback across Different Environments , March 2019 , pp. 175 - 177
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

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