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High-energy emission from the eclipsing millisecond pulsar PSR 1957+20The 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.
Document ID
19930039976
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Arons, Jonathan
(NASA Headquarters Washington, DC United States)
Tavani, Marco
(California Univ. Berkeley; Lawrence Livermore National Lab., Livermore, United States)
Date Acquired
August 16, 2013
Publication Date
January 20, 1993
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 403
Issue: 1
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
93A23973
Funding Number(s)
CONTRACT_GRANT: NSF AST-91-15093
CONTRACT_GRANT: W-7405-ENG-48
CONTRACT_GRANT: NAGW-2413
Distribution Limits
Public
Copyright
Other

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