Search for TeV gamma-ray emission from binary radio pulsars

Details Search for TeV gamma-ray emission from binary radio pulsars Search for TeV gamma-ray emission from binary radio pulsars

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...444..419r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 444, no. 1, p. 419-423

Astronomy and Astrophysics

Astronomy

Binary Stars, Emission Spectra, Gamma Ray Astronomy, Gamma Rays, Pulsars, Stellar Radiation, Pulses, Radio Emission, Shock Fronts, Stellar Winds, Wave Scattering

Scientific paper

Results of a TeV gamma-ray survey of six binary radio pulsars are presented. One of the objects, namely PSR B1855+09, showed orbitally modulated, pulsed emission with a probability due to chance of 1 x 10-2 in the orbital phase range 0.15-0.25. The emission pattern is similar to the radio emission, although the double peak seems to show some structure. No confirmation of the reported DC emission at the L4 position in the orbit from PSR B1957+20 could be found, indicating an energy cutoff at a few TeV. A model is proposed whereby orbitally modulated TeV gamma ray emission could be produced in this system: Accelerated electrons from the pulsar wind will produce TeV gamma rays through inverse-Compton scattering in the curved shock surrounding the comapanion star. Doppler boosting along the shock front results in a maximum gamma ray energy of 6 TeV, and emission in a narrow angle in the general directions of L4 and L5. The maximum predicted luminosity is slightly less than measured by Brink et al. (1990).

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