Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...435..218m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 435, no. 1, p. 218-224
Astronomy and Astrophysics
Astronomy
26
Astronomical Models, Gamma Ray Astronomy, Globular Clusters, Pulsars, Sky Surveys (Astronomy), Spaceborne Astronomy, Star Formation, Stellar Winds, Gamma Ray Observatory, Gamma Ray Telescopes, Mathematical Models, Maximum Likelihood Estimates, Relativistic Electron Beams
Scientific paper
We report upper limits to the high-energy gamma-ray emission from the millisecond pulsars (MSPs) in a number of globular clusters. The observations were done as part of an all-sky survey by the energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory (CGRO) during Phase I of the CGRO mission (1991 June to 1992 November). Several theoretical models suggest that MSPs may be sources of high-energy gamma radiation emitted either as primary radiation from the pulsar magnetosphere or as secondary radiation generated by conversion into photons of a substantial part of the relativistic e(+/-) pair wind expected to flow from the pulsar. To date, no high-energy emission has been detected from an individual MSP. However, a large number of MSPs are expected in globular cluster cores where the formation rate of accreting binary systems is high. Model predictions of the total number of pulsars range in the hundreds for some clusters. These expectations have been reinforced by recent discoveries of a substantial number of radio MSPs in several clusters; for example, 11 have been found in 47 Tucanae (Manchester et al.). The EGRET observations have been used to obtain upper limits for the efficiency eta of conversion of MSP spin-down power into hard gamma rays. The upper limits are also compared with the gamma-ray fluxes predicted from theoretical models of pulsar wind emission (Tavani). The EGRET limits put significant constraints on either the emission models or the number of pulsars in the globular clusters.
Bertsch David L.
Brazier K.
Chiang James
Dingus Brenda Lynn
Fichtel Carl E.
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