Hostname: page-component-7bb8b95d7b-lvwk9 Total loading time: 0 Render date: 2024-09-17T15:20:07.956Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetic Fields and Cosmic Rays in Galaxy Clusters

Published online by Cambridge University Press:  21 October 2010

Klaus Dolag
Klaus Dolag*
Affiliation:
MPI for Astrophysic, Karl-Schwarzchild-Str. 1, D-85741 Garching, Germany
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.

In galaxy clusters, non-thermal components such as magnetic field and high energy particles keep a record of the processes acting since early times till now. These components play key roles by controlling transport processes inside the cluster atmosphere and beyond and therefore have to be understood in detail by means of numerical simulations. The complexity of the intra cluster medium revealed by multi-frequency observations demonstrates that a variety of physical processes are in action and must be included properly to produce accurate and realistic models. Confronting the predictions of numerical simulations with observations allows us to validate different scenarios about origin and evolution of large scale magnetic fields and to investigate their role in transport and acceleration processes of cosmic rays.

Keywords

magnetic fieldsmethods: numericalgalaxies: clusters: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 461 - 463
Copyright
Copyright © International Astronomical Union 2010

References

Carilli, C. T. & Taylor, G. B. 2002, ARAA, 40, 319CrossRefGoogle Scholar
Clarke, T. E., Kronberg, P. P., & Boehringer, H.ApJ, 547, L111CrossRefGoogle Scholar
Dolag, K., Bykov, A. M., & Diaferio, A. 2008, SSRev, 134, 311Google Scholar
Dolag, K., Bratelmann, M., & Lesch, H. 1999, A&A, 348, 351Google Scholar
Dolag, K., Bratelmann, M., & Lesch, H. 2002, A&A, 387, 383Google Scholar
Dolag, K. & Ensslin, T. 2000 A&A, 362, 151Google Scholar
Dolag, K., Grasso, D., Springel, V., & Tkachev, I. 2005, Journal of Cosmology and Astro-Particle Physics, 1, 9CrossRefGoogle Scholar
Dolag, K. & Stasyszyn, F. 2009, MNRAS, 398, 1678CrossRefGoogle Scholar
Donnert, R., Dolag, K., Lesch, H., & Mueller, E. 2009, MNRAS, 292, 1008CrossRefGoogle Scholar
Donnert, R., Dolag, K., Cassano, R., & Brunetti, G., MNRAS, in pressGoogle Scholar
Donnert, R., Dolag, K., Brunetti, G., & Cassano, R., in prepGoogle Scholar
Ferrari, C., Govoni, F., Schindler, S., Bykov, A. M., & Rephaeli, Y. 2008, SSRev, 134, 93Google Scholar
Govoni, F. & Feretti, L. 2004, International Journal of Modern Physics D, 13, 1549CrossRefGoogle Scholar
Miniatti, F., Johns, T. W., Kang, H., & Ryu, D. 2001, ApJ, 512, 233CrossRefGoogle Scholar
Pfrommer, C., Ensslin, T. A., Jubelgas, M., Springel, & Dolag, K. 2007 MNTAS, 378, 385CrossRefGoogle Scholar