Detectability of g-Ray from Millisecond Pulsars with MAGIC

Details Detectability of g-Ray from Millisecond Pulsars with MAGIC Detectability of g-Ray from Millisecond Pulsars with MAGIC

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....4.2457o&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

Scientific paper

Beside the so called canonical pulsars, a sample of radio pulsars, the millisecond pulsars, have been detected with rotational periods in the range from 1 ms to 10 ms. These pulsars are rather old, and most probably have been recycled by some external mechanism (usually a binary system). The surface magnetic fields are lower than that of canonical pulsars, with Bs ˜ 109 G. Given such a low magnetic field, the cut-off energy of curvature photons due to pair production shifts to higher energies since the condition for pair production on the perpendicular component of the fiel is Eγ B⊥ ≥ 1018.6 [3]. Moreover, millisecond pulsars are expected to radiate mostly in the range between 10 GeV and 1.5 TeV, as discussed in the paper. The Cherenkov telescope MAGIC with the energy threshold of ˜ 30 GeV will therefore be able to determine the nature of these objects. The detection rates discussed in this paper make no assumption about hadron rejection capability.

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