Emission of Kepler's Supernova Remnant Produced by Accelerated Cosmic Rays

Berezhko, Evgeni; Ksenofontov, Leonid; Völk, Heinrich

Item

ITEM ACTIONSEXPORT

Add to Basket

Local TagsRelease HistoryDetailsSummary

Released

Conference Paper

Emission of Kepler's Supernova Remnant Produced by Accelerated Cosmic Rays

MPS-Authors

/persons/resource/persons31141

Völk, Heinrich
Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society;

External Resource

No external resources are shared

Fulltext (restricted access)

There are currently no full texts shared for your IP range.

Fulltext (public)

There are no public fulltexts stored in PuRe

Supplementary Material (public)

There is no public supplementary material available

Citation

Berezhko, E., Ksenofontov, L., & Völk, H. (2005). Emission of Kepler's Supernova Remnant Produced by Accelerated Cosmic Rays. In J. Blümer (Ed.), Contributions to the 29th International Cosmic Ray Conference, Pune, India, 2005 (pp. 227-230). Karlsruhe: Forschungszentrum Karlsruhe.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0011-876F-0

Abstract

The nonlinear kinetic model of cosmic ray acceleration in supernova remnants (SNRs) is used to describe the properties of the Kepler's SNR. The calculated expansion law and the radio and X-ray emission produced by the accelerated cosmic rays in Kepler's SNR agree quite well with the observations. A rather large interior magnetic field about 200 μG is required to give a good fit for the radio and X-ray synchrotron emission. The predicted TeV gamma-ray emission, which is of hadronic origin, is expected at a detectable level.