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Non-variable cosmologically distant gamma-ray emitters as an imprint of propagation of ultra-high-energy protons

MPG-Autoren

Prosekin,  A. Yu.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons30663

Kelner,  Stanislav R.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

Aharonian,  F. A.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;
Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland;

Externe Ressourcen
Volltexte (frei zugänglich)

1105.1947
(Preprint), 165KB

Ergänzendes Material (frei zugänglich)
Es sind keine frei zugänglichen Ergänzenden Materialien verfügbar
Zitation

Prosekin, A. Y., Kelner, S. R., & Aharonian, F. A. (2011). Non-variable cosmologically distant gamma-ray emitters as an imprint of propagation of ultra-high-energy protons. Astrophysics & Astronomy, 536: A30, pp. 1-7.


Zitierlink: http://hdl.handle.net/11858/00-001M-0000-000F-1000-F
Zusammenfassung
The acceleration cites of ultra-high-energy (UHE) protons can be traced by the footprint left by these particles propagating through cosmic microwave background (CMB) radiation. Secondary electrons produced in extended region of several tens of Mpc emit their energy via synchrotron radiation predominantly in the initial direction of the parent protons. It forms a non-variable and compact (almost point-like) source of high energy gamma rays. The importance of this effect is increased for cosmologically distant objects; because of severe energy losses, UHE protons cannot achieve us even in the case of extremely weak intergalactic magnetic fields. Moreover, at high redshifts the energy conversion from protons to secondary particles becomes significantly more effective due to the denser and more energetic CMB in the past. This increases the chances of UHE cosmic rays to be traced by the secondary synchrotron gamma radiation. We discuss the energy budget and the redshift dependence of the efficiency of energy transfer from UHE protons to synchrotron radiation. The angular and spectral distributions of radiation in the gamma- and X-ray energy bands are calculated and discussed in the context of their detectability by Fermi LAT and Chandra observatories.