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2011

New developments in the ancient PulsarWind Nebulae scenario

Tibolla, O., Mannheim, K., Kaufmann, S. et al.

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In a Pulsar Wind Nebula (PWN), the lifetime of inverse Compton emitting electrons exceeds the lifetime of its progenitor pulsar, but it exceeds also the age of the electrons that emit via synchrotron radiation; i.e.

while the PWN grows older, it can remain bright in IC, whereas its GeV-TeV gamma-ray (for $10^5-10^6$ years) flux remains high for timescales much larger than the Pulsar lifetime and the PWN visible in X-rays.
The shell-type remnant of the supernova explosion that led to the formation of the pulsar also has a much shorter lifetime.
In this scenario, the magnetic field in the cavity induced by the wind of the progenitor star plays a crucial role, but also the magnetic field in the interstellar medium cannot be negligible and its outward decrease away from the Galactic disk further reduces their X-ray brightness.

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