Implications for the detection of ultra-high-energy gamma rays from SCO X-1

Details Implications for the detection of ultra-high-energy gamma rays from SCO X-1 Implications for the detection of ultra-high-energy gamma rays from SCO X-1

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...219l...1m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 219, no. 1-2, July 1989, p. L1, L2.

Astronomy and Astrophysics

Astronomy

4

Emission Spectra, Gamma Ray Astronomy, Pulsars, X Ray Binaries, Galactic Bulge, Particle Acceleration, Stellar Luminosity, Stellar Magnetic Fields, Stellar Mass Accretion

Scientific paper

Ultrahigh energy (UHE) gamma-ray emission can be either due to a direct pulsar type mechanism or preceded by UHE particle acceleration. Whereas for isolated pulsars or millisecond binary radio pulsars, the acceleration mechanism is almost obvious there exists a great degree of uncertainty as to the mechanism responsible for the acceleration of particles to UHE region in the luminous X-ray binaries. Use is made of the fact that the neutron star of Sco X-1 is perhaps old with a magnetic field less than 10 to the 9th G to infer that the recently proposed improved dynamo mechanism or the shock acceleration is the most likely mechanism at work.

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