Einleitung

Böttcher, Jörg

doi:10.1007/978-3-642-40112-1_1

Cited by 1 publication

(1 citation statement)

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“…In the case of the binary system PSR B1259-63, the decretion disk extends up to the distance of the pulsar periastron. In such a case, gamma-ray emission above the ∼TeV energy range can be also produced in the comptonization of the disk radiation [63,64]. If this also occurs for the binary system considered here, then the steady, extended TeV emission from the HEGRA TeV γ-ray source (TeV J2032+4130) can be overcome by the point-like emission from the binary system also above a few TeV during the periastron passage of the pulsar.…”

Section: Figures (A)mentioning

confidence: 84%

Gamma-rays from the binary system containing PSR J2032+4127 during its periastron passage

Bednarek¹,

Banasiński²,

Sitarek³

2017

J. Phys. G: Nucl. Part. Phys.

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Abstract. The energetic pulsar, PSR J2032+4127, has been recently discovered in the direction of the unidentified HEGRA TeV γ-ray source (TeV J2032+4130). It is proposed that this pulsar forms a binary system with the Be type star, MT91 213, expected to reach the periastron late in 2017. We performed detailed calculations of the γ-ray emission produced close to the binary system's periastron passage by applying a simple geometrical model. Electrons accelerated at the collision region of pulsar and stellar winds initiate anisotropic Inverse Compton e ± pair cascades by scattering soft radiation from the massive companion. The γ-ray spectra, from such a comptonization process, are confronted with the measurements of the extended TeV γ-ray emission from the HEGRA TeV γ-ray source. We discuss conditions within the binary system, at the periastron passage of the pulsar, for which the γ-ray emission from the binary can overcome the extended, steady TeV γ-ray emission from the HEGRA TeV γ-ray source.

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Section: Figures (A)mentioning

confidence: 84%