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Variable Very-High-Energy Gamma-Ray Emission from the Microquasar LS I +61 303

Microquasars are binary star systems with relativistic radio-emitting jets. They are potential sources of cosmic rays and can be used to elucidate the physics of relativistic jets. We report the detection of variable gamma-ray emission above 100 gigaelectron volts from the microquasar LS I 61 + 303....

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Bibliographic Details
Published in:Science (American Association for the Advancement of Science) 2006-06, Vol.312 (5781), p.1771-1773
Main Authors: Aliu, E, Anderhub, H, Antoranz, P, Armada, A, Asensio, M, Baixeras, C, Bartelt, M, Bavikadi, S.R, Bednarek, W, Bigongiari, C, Biland, A, Bock, R.K, Bordas, P, Bosch-Ramon, V, Bretz, T, Camara, M, Carmona, E, Commichau, S, Contreras, J.L, Curtef, V, Danielyan, V, De Angelis, A, De Lotto, B, Dorner, D, Errando, M, Firpo, R, Fonseca, M.V, Font, L, Fuchs, M, Garczarczyk, M, Gaug, M, Giller, M, Hakobyan, D, Hengstebeck, T, Höhne, D, Hose, J, Isar, P.G, Jacon, P, Kranich, D, Laatiaoui, M, Laille, A, Lenisa, T, Lindfors, E, Lombardi, S, Longo, F, López, M, Lorenz, E, Lucarelli, F, Majumdar, P, Mansutti, O, Martínez, M, Mase, K, Mazin, D, Merck, C, Meyer, M, Miranda, J.M, Mirzoyan, R, Mizobuchi, S, Moralejo, A, Nilsson, K, Oña-Wilhelmi, E, Otte, N, Paneque, D, Paredes, J.M, Pascoli, D, Persic, M, Poller, M, Prandini, E, Rhode, W, Ribó, M, Rico, J, Robert, A, Romero, G.E, Rügamer, S, Saggion, A, Sartori, P, Scalzotto, V, Scapin, V, Schmitt, R, Schweizer, T, Shayduk, M, Shore, S.N, Sidro, N, Sobczynska, D, Stamerra, A, Stark, L.S, Takalo, L, Temnikov, P, Tescaro, D, Teshima, M, Tonello, N, Torres, D.F, Turini, N, Vankov, H, Vitale, V, Wagner, R.M, Wibig, T, Wittek, W, Zanin, R, Zapatero, J
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Language:English
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Summary:Microquasars are binary star systems with relativistic radio-emitting jets. They are potential sources of cosmic rays and can be used to elucidate the physics of relativistic jets. We report the detection of variable gamma-ray emission above 100 gigaelectron volts from the microquasar LS I 61 + 303. Six orbital cycles were recorded. Several detections occur at a similar orbital phase, which suggests that the emission is periodic. The strongest gamma-ray emission is not observed when the two stars are closest to one another, implying a strong orbital modulation of the emission or absorption processes.
ISSN:0036-8075
1095-9203
DOI:10.1126/science.1128177