Modelling of far ultraviolet emission of pulsar wind nebulae with bow shocks

Abstract

Abstract The kinetic modelling of electron and positron acceleration in the colliding shock flows of pulsar wind nebulae with bow shocks allows to explain the nature of their hard particle spectra. The hard synchrotron emission produced by the accelerated particles can reach the far ultraviolet range (1250 — 2000 Å) providing the maximal luminosity of the bow shock nebulae in this range. In this paper the results of modelling of pulsar wind particles transport in the colliding shock flows in the bow shock nebulae of PSRs J1741-2054 and B1929+10 are presented. The results of the synchrotron emission modelling are confronted to the observations in order to estimate possible far ultraviolet luminosities of the discussed objects.