Acceleration and evolution of cosmic ray electrons during radio-galaxy-cluster-shock encounters

Thomas W Jones, B. J. O'Neill, C. Nolting, P. J. Mendygral

Research output: Contribution to journalConference articlepeer-review


Radio Galaxies (radio-loud AGNs, or RGs) are common in galaxy cluster media (ICMs). In addition to their potential thermodynamical roles, these RGs may also serve to illuminate important ICM dynamical features, especially ICM shocks. Those interactions are revealed most clearly by radio synchrotron emissions from associated RG Cosmic Ray Electrons (CRe). Here we report results from "MHD+CR" simulations of RG-shock encounters and specifically on resultant shock acceleration (DSA) of the CRe and observable consequences. We find, in particular, that even modest-strength ICM shocks (Ms ∼3-4) may lead to significant and observable DSA of the RG CRe. This work has impact on both the nature of large scale cluster radio emissions, including so-called radio relics and our understanding of RG-ICM-shock dynamics.

Original languageEnglish (US)
JournalProceedings of Science
StatePublished - Jan 1 2017
Event35th International Cosmic Ray Conference, ICRC 2017 - Bexco, Busan, Korea, Republic of
Duration: Jul 10 2017Jul 20 2017

Bibliographical note

Funding Information:
Acknowledgments This work at the University of Minnesota was supported in part by NSF grant AST1211595. The reported simulations utilized high performance resources made available by the University of Minnesota Supercomputing Institute.

Publisher Copyright:
© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-Non Commercial-No Derivatives 4.0 International License (CC BY-NC-ND 4.0).


Dive into the research topics of 'Acceleration and evolution of cosmic ray electrons during radio-galaxy-cluster-shock encounters'. Together they form a unique fingerprint.

Cite this