Unidentified Gamma-Ray Sources as Ancient Pulsar Wind Nebulae
Abstract
In this paper we explore the evolution of a PWN while the pulsar is spinning down. An MHD approach is used to simulate the evolution of a composite remnant. Particular attention is given to the adiabatic loss rate and evolution of the nebular field strength with time. By normalising a two component particle injection spectrum (which can reproduce the radio and X-ray components) at the pulsar wind termination shock to the time dependent spindown power, and keeping track with losses since pulsar/PWN/SNR birth, we show that the average field strength decreases with time as , so that the synchrotron flux decreases, whereas the IC gamma-ray flux increases, until most of the spindown power has been dumped into the PWN. Eventually adiabatic and IC losses will also terminate the TeV visibility and then eventually the GeV visibility.
Keywords
Cite
@article{arxiv.0906.2644,
title = {Unidentified Gamma-Ray Sources as Ancient Pulsar Wind Nebulae},
author = {O. C. de Jager and S. E. S. Ferreira and A. Djannati-Ataï and M. Dalton and C. Deil and K. Kosack and M. Renaud and U. Schwanke and O. Tibolla},
journal= {arXiv preprint arXiv:0906.2644},
year = {2009}
}
Comments
Submissions to the 31st International Cosmic Ray Conference, Lodz, Poland, July 2009, four pages