O. Tibolla, K. Mannheim, D. Elsässer, S. Kaufmann
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. during the
evolution of the PWN, 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 in which the pulsar was formed 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. This is in line with the
discovery of several unidentified sources in the TeV gamma-ray band without
X-ray counterparts. Moreover, the consequences are important also in order to
reinterprete the detection of starburst galaxies in the TeV gamma-ray band
considering a leptonic origin of the gamma-ray signal.
View original:
http://arxiv.org/abs/1111.1634
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