Secondary Photons from High-energy Protons Accelerated in Hypernovae

Details Secondary Photons from High-energy Protons Accelerated in Hypernovae Secondary Photons from High-energy Protons Accelerated in Hypernovae

2008-03-15

arxiv.org/abs/0803.2280v1

Astrophys.J.677:L31-L34, 2008

Astronomy and Astrophysics

Astrophysics

Accepted by ApJL

Scientific paper

10.1086/587963

Recent observations show that hypernovae may deposit some fraction of their kinetic energy in mildly relativistic ejecta. In the dissipation process of such ejecta in a stellar wind, cosmic ray protons can be accelerated up to $\sim 10^{19}$ eV. We discuss the TeV to MeV gamma-ray and the X-ray photon signatures of cosmic rays accelerated in hypernovae. Secondary X-ray photons, emitted by electron-positron pairs produced via cascade processes due to high-energy protons, are the most promising targets for X-ray telescopes. Synchrotron photons emitted by protons can appear in the GeV band, requiring nearby ($<40$ Mpc) hypernovae for detection with GLAST. In addition, air Cherenkov telescopes may be able to detect regenerated TeV photons emitted by electron-positron pairs generated by CMB attenuation of $\pi^0$ decay photons.

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