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Shock geometry and inverse Compton emission from the wind of a binary pulsar
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Shock geometry and inverse Compton emission from the
wind of a binary pulsar
Lewis Ball Jennifer Dodd
To appear in Publ. Astronomical Soc. Aust. 18/1
Submitted 19 Jul. 2000; Revised 8 Nov. 2000; Accepted 13 Nov. 2000
Research Centre for Theoretical Astrophysics, University of Sydney, N.S.W. 2006, Australia
ball@physics.usyd.edu.au
Abstract
PSR B1259?63 is a 47ms radio pulsar with a high spin-down luminosity which is in a
close, highly eccentric 3.5-year orbit about a bright stellar companion. The binary system
may be a detectable source of hard γ-rays produced by inverse Compton scattering of pho-
tons from the B2e star SS2883 by electrons and positrons in the pulsar wind. The star
provides an enormous density of optical photons in the vicinity of the pulsar, particularly at
epochs near periastron. We calculate the emission from the unshocked region of the pulsar
wind, assuming that it terminates at a shock where it attains pressure balance with the
companion’s wind. The spectra and light curves for the inverse Compton emission from the
shock-terminated wind are compared with those for an unterminated wind. If the pulsar’s
wind is weaker than that from the companion star, the termination of the wind decreases the
inverse Compton flux, particularly near periastron. The termination shock geometry has the
effect of decreasing the asymmetry of the γ-ray light curve around periastron, which arises
because of the asymmetrical variation of the scattering angle.
Keywords: Pulsars; Inverse Compton scattering; Gamma-rays; Cherenkov telescopes; Pul-
sars: individual (PSR B1259?63)
1 Introduction
PSR B1259?63 is one of only three known radio pulsars which have a main sequence star binary
companion. Such systems provide a unique environment for inverse Compton scattering because
of the presence of an enormous density of low energy (optical) photons which serve as targets for
electrons and positrons in the pul
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