Photon–photon pair production and the opacity of SN1987A to TeV and PeV γ-rays

Protheroe, R. J.

doi:10.1038/329135a0

Cited by 12 publications

(2 citation statements)

References 17 publications

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“…In the case of γ-ray production, a significant fraction of the γ-rays will interact by pair production with target nuclei in the shell and will not be observed. Also, during the first few months, TeV γ-rays could interact with radiation from the photosphere of the supernova [47]. By several days after the explosion, the radius of the photosphere becomes smaller than that of the SNR shell, where the neutrons interact, and continues to decrease in radius relative to the shell.…”

Section: Spectrum Of Neutrons From Photodisintegration Of Fe Nucleimentioning

confidence: 99%

Gamma-rays and neutrinos from very young supernova remnants

Protheroe

Bednarek

Luo

1998

Astroparticle Physics

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We consider the result of acceleration of heavy ions in the slot gap potential of a very young pulsar with a hot polar cap. Photodisintegration of the heavy ions in the radiation field of the polar cap and pulsar surface gives rise to a flux of energetic neutrons. Some fraction of these neutrons interact with target nuclei in the supernova shell to produce neutrino and gamma-ray signals which should be observable from very young supernova remnants in our galaxy for a range of pulsar parameters.

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Section: Spectrum Of Neutrons From Photodisintegration Of Fe Nucleimentioning

confidence: 99%

Gamma-rays and neutrinos from very young supernova remnants

Protheroe

Bednarek

Luo

1998

Astroparticle Physics

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show abstract

“…Such a pulsar and nebula will inevitably contribute Aux at other wavelengths as well, and more detailed modeling is required to decide whether it can also fit with the observed light curve, 'the independent (y-ray) evidence for radiogenic energy input, and so forth. (Berezinsky and Ginzberg, 1987;Honda andMori, 1987a, 1987b;Protheroe, 1987). There is at most very marginal evidence for a TeV flux of about 3X10 ergs/s at the time of the January soft-x-ray flare (Kifune, 1988 (Srinivasan, 1985).…”

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confidence: 98%