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ɣ-Ray Emission from Slow Pulsars

Published online by Cambridge University Press:  14 August 2015

M. Morini  and
A. Treves
M. Morini
Affiliation:
Istituto di Fisica dell'Università and L.F.C.T.R., Milano, Italy
A. Treves
Affiliation:
Istituto di Fisica dell'Università and L.F.C.T.R., Milano, Italy

Extract

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Among the COS-B Galactic γ-ray sources two have been identified with the young pulsars PSR0531+21 and PSR0833–45, while for most of the others there are no convincing counterparts. An obvious explanation is that at least part of them are also pulsars. Because of the rarity of pulsar formation, an important issue for testing this possibility is to discuss whether relatively old pulsars (~105y) may be sources of γ-rays of the luminosity observed by COS-B (φ (100 MeV) 10−6cm−2s−1). On this line it is of great interest the claim of observation of γ-rays with SAS II from PSR1747–46 and with COS-B from PSR0740–28 and PSR1822–09, communicated at other conferences, but yet not confirmed. The three slow pulsars mentioned above were reported to have γ-ray luminosities of 1033 erg s−1 close to their intrinsic energy loss LT = Iωω. Their periods are about 0.1–1s and their distance ~1 Kpc.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 94: Origin of Cosmic Rays , 1981 , pp. 205 - 206
Copyright
Copyright © Reidel 1981 

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