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Search for Pulsed VHE γ-ray Emission from Young Pulsars with H.E.S.S.

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Konopelko,  Alexander
Prof. Heinrich J. Völk, Emeriti, MPI for Nuclear Physics, Max Planck Society;

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Citation

Konopelko, A., Chadwick, P., Eifert, T., Lohse, T., Noutsos, A., Rayner, S., et al. (2005). Search for Pulsed VHE γ-ray Emission from Young Pulsars with H.E.S.S. In B. S. Acharya, S. Gupta, P. Jagadeesan, A. Jain, S. Karthikeyan, S. Morris, et al. (Eds.), Proceedings of the 29th International Cosmic Ray Conference (pp. 139-142). Navy Nagar, Colaba, Mumbai, MH-400005: Tata Institute of Fundamental Research.


Cite as: https://hdl.handle.net/11858/00-001M-0000-0011-878D-C
Abstract
Pulsars are commonly regarded as highly magnetized neutron stars, rotating up to several hundred times per second. Over 1,500 radio pulsars have been found so far, about 70 of which are X-ray pulsars, but only a handful have been observed in γ-rays. This high-energy emission is believed to be produced by the electrons accelerated to TeV energies in the pulsar magnetosphere, resulting in cascades of secondary particles. The H.E.S.S. experiment is a system of four imaging atmospheric Cherenkov telescopes in Namibia, which is sensitive to γ-rays above 100 GeV. Three young pulsars, Crab, Vela, and PSR B1706-44 have been observed with H.E.S.S. The results of the search for pulsed emission for these targets, and the constraints on the theories of pulsed very high energy γ-ray emission, are summarized here.