High-energy emission from the eclipsing millisecond pulsar PSR 1957+20

Details High-energy emission from the eclipsing millisecond pulsar PSR 1957+20 High-energy emission from the eclipsing millisecond pulsar PSR 1957+20

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...403..249a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 403, no. 1, p. 249-255.

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79

Computational Astrophysics, Eclipsing Binary Stars, Emission Spectra, Pulsars, Nebulae, Shock Waves, Stellar Models, Stellar Winds

Scientific paper

The properties of the high-energy emission expected from the eclipsing millisecond pulsar system PSR 1957+20 are investigated. Emission is considered by both the relativistic shock produced by the pulsar wind in the nebula surrounding the binary and by the shock constraining the mass outflow from the companion star of PSR 1957+20. On the basis of the results of microscopic plasma physical models of relativistic shocks it is suggested that the high-energy radiation is produced in the range from X-rays to MeV gamma rays in the binary and in the range from 0.01 eV to about 40 keV in the nebula. Doppler boost of the emission in the radiating wind suggests the flux should vary on the orbital time scale, with the largest flux observed roughly coincident with the pulsar's radio eclipse.

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