Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2009-06-15
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
Submissions to the 31st International Cosmic Ray Conference, Lodz, Poland, July 2009, four pages
Scientific paper
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 $t^{-1.3}$, 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.
Dalton M. M.
de Jager Ocker C.
Deil Christoph
Djannati-Ataï Arache
Ferreira S. E. S.
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