Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-10T16:41:26.372Z Has data issue: false hasContentIssue false
  • English
  • Français

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: stela.faria@usp.br
Elisabete M. de Gouveia Dal Pino
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, University of São Paulo (USP), São Paulo, Brazil e-mail: stela.faria@usp.br
Paramita Barai
Affiliation:
Núcleo de Astrofísica - Universidade Cruzeiro do Sul (NAT - UNICSUL), São Paulo, Brazil
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

References

Alves Batista, R., Saveliev, A., & de Gouveia Dal Pino, E. M. 2019, MNRAS, 489, 3836 Google Scholar
Barai, P. & de Gouveia Dal Pino, E. M. 2019, MNRAS, 487, p.5549–5563 CrossRefGoogle Scholar
de Gouveia Dal Pino, E. M. 2011, ISBN 978-1-908106-12 Hardback, pp.37–52 Google Scholar
Dolag, K. & Stasyszyn, F. 2009, MNRAS, 398, 1678 CrossRefGoogle Scholar
Fermi-LAT Collaboration, 2018, ApJS, 237, 36 CrossRefGoogle Scholar
Grasso, D. & Rubinstein, H. R. 2001, Phys. Rep., 348, 163–266 10.1016/S0370-1573(00)00110-1CrossRefGoogle Scholar
Marinacci, F. et al. 2018, MNRAS, 480, 5113M Google Scholar
Santos-Lima, R. et al. 2014, ApJ, 781, 84 CrossRefGoogle Scholar