Abstract
High-energy pulsars typically show a power-law spectrum in CGRO/EGRET energy band with photon spectral indices ranging from -1.4 to -1.8. This is most likely to be produced by a cooling (via a dominant radiation mechanism) population of charges. A spectral bending energy, below which the power law does not continue to extend, can be used to determine the emission location and mechanisms of these high-energy emissions. We report recent RXTE observation results of PSR B0656+14 and PSR B1951+32 in this respect, which favor an outer magnetosphere emission location, We then discuss the importance of INTEGRAL'S observation of high-energy pulsars in solving the essential issue of modelling high-energy emission from pulsars. © 1999 OPA (Overseas Publishers Association) N.V. Published by license under the Gordon and Breach Science Publishers imprint.