ausblenden:
Schlagwörter:
-
MPINP:
HESS - Abteilung Hofmann
Zusammenfassung:
One of the most prominent classes of astrophysical particle accelerators are su-
pernova remnants. These objects result from the interaction of stellar material,
being ejected during supernova explosions at velocities of several thousands of
kilometres per second, with the ambient medium. The H.E.S.S. experiment is
able to observe such sources at very-high-energies (
>
100 GeV) with the best
possible sensitivity to date. As a first part of this work, a simulation of the
theoretically expected population of supernova remnants at these energies was
performed, followed by an analysis of the very-high-energy gamma-ray emis-
sion from the source ensemble known at other wave lengths. Assuming cur-
rently accepted standard parameters, the simulation is able to reproduce the
observed numbers of supernova remnants in the radio as well as the very-high-
energy range, but only if these objects amplify their own magnetic field. It
should be mentioned, however, that a large number of parameters is required
in the simulation, many of which are attributed with large uncertainties. The
data analysis did not result in any new detections but allowed it to determine
over a hundred flux upper limits. A hint of a faint, cumulated emission from
the ensemble of supernova remnants might have been observed. A comparison
to the developed model gives an explanation for the gamma-ray faintness of the
investigated objects and suggests a possible detection of over a hundred super-
nova remnants with the next generation of Cherenkov telescope experiments.