Abstract
Since their discovery, pulsars have been observed in a wide range of wavelengths. The development of several theoretical models of emission have been proposed from these data. The EGRET detector of the CGRO satellite detected pulsed emission from several high energy pulsars (at the limit of its sensibility, with energies below 20 GeV). The energy band between 15 – 300 GeV is at present unexplored. Forthcoming ground-based Cherenkov telescope MAGIC (Major Atmospheric Gamma Imaging Cherenkov telescope) will be able to observe below 100 GeV. MAGIC will see its first light in Sept. 2002. Here we summarize (using theoretical simulations) the MAGIC sensibility for pulsar detection and its possible contribution to the actual theoretical models which predict different cut-offs, for γ emission in the energy range between high energies (up to 10 GeV) and very high energies (up to 100 TeV).
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