ACKERMANN, Markus; AJELLO, Marco; BALLET, Jean; BARBIELLINI, Guido; BASTIERI, D.; BELLAZZINI, R.; BONAMENTE, E.; J. BRANDT, T.; BREGEON, J.; BRIGIDA, M.; BRUEL, Pascal; BUEHLER, R.; BUSON, S.; A. CALIANDRO, G.; A. CAMERON, R.; CARAVEO, P. A.; M. CASANDJIAN, J.; CAVAZZUTI, E.; CECCHI, C.; CHEKHTMAN, A.; CHIANG, J.; CHIARO, G.; CIPRINI, S.; CLAUS, R.; COHEN-TANUGI, J.; R. COMINSKY, L.; CONRAD, J.; CUTINI, S.; DALTON, M.; D'AMMANDO, F.; DE ANGELIS, A.; R. DEN HARTOG, P.; DE PALMA, F.; D. DERMER, C.; W. DIGEL, S.; DI VENERE, L.; S. DRELL, P.; DUBOIS, R.; FAVUZZI, C.; J. FEGAN, S.; C. FERRARA, E.; B. FOCKE, W.; FRANCKOWIAK, A.; FUNK, S.; FUSCO, P.; GARGANO, F.; GASPARRINI, D.; GERMANI, S.; GIGLIETTO, N.; GIORDANO, F.; GIROLETTI, M.; GLANZMAN, T.; GODFREY, G.; A. GRENIER, I.; GUIRIEC, S.; HADASCH, D.; HANABATA, Y.; K. HARDING, A.; HAYASHIDA, M.; HAYS, E.; B. HILL, A.; HORAN, D.; E. HUGHES, R.; JOGLER, T.; J ́OHANNESSON, G.; JOHNSON, A.S.; J. JOHNSON, T.; KAWANO, T.; KERR, M.; KN ̈ODLSEDER, J.; KUSS, M.; LANDE, J.; LARSSON, S.; LATRONICO, L.; LEMOINE-GOUMARD, M.; LI, J.; LONGO, F.; N. LOVELLETTE, M.; LUBRANO, P.; MAYER, M.; N. MAZZIOTTA, M.; E. MCENERY, J.; F. MICHELSON, P.; MIZUNO, T.; E. MONZANI, M.; MORSELLI, A.; V. MOSKALENKO, I.; MURGIA, S.; NEMMEN, R.; NUSS, E.; OHSUGI, T.; OKUMURA, A.; ORIENTI, M.; ORLANDO, E.; F. ORMES, J.; PANEQUE, D.; PAPITTO, A.; S. PERKINS, J.; PESCE-ROLLINS, M.; PIRON, F.; PIVATO, G.; RAIN'O, S.; RANDO, R.; RAZZANO, M.; REA, N.; REIMER, A.; REIMER, O.; D. SCARGLE, J.; SCHULZ, A.; SGR'O, C.; J. SISKIND, E.; SPANDRE, G.; SPINELLI, P.; TAKAHASHI, H.; G. THAYER, J.; B. THAYER, J.; TINIVELLA, M.; F. TORRES, D.; TOSTI, G.; TROJA, E.; UCHIYAMA, Y.; L. USHER, T.; VANDENBROUCKE, J.; VASILEIOU, V.; VIANELLO, G.; VITALE, V.; WERNER, M.; L. WINER, B.; S. WOOD, K.

doi:10.1088/2041-8205/773/2/L35

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ACKERMANN, Markus

AJELLO, Marco

BALLET, Jean
Astrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]

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The Astrophysical journal letters. 2013, vol. 773, p. L35

Bristol : IOP Publishing

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Gamma-ray binaries are stellar systems for which the spectral ene rgy distribu- tion (discounting the thermal stellar emission) peaks at high energie s. Detected from radio to TeV gamma rays, the γ -ray binary LS I +61 ◦ 303 is highly variable across all frequencies. One aspect of this system's variability is the modula- tion of its emission with the timescale set by the ∼ 26 . 4960-day orbital period. Here we show that, during the time of our observations, the γ -ray emission of LS I +61 ◦ 303 also presents a sinusoidal variability consistent with the previou sly- known superorbital period of 1667 days. This modulation is more pro minently seen at orbital phases around apastron, whereas it does not intr oduce a visible change close to periastron. It is also found in the appearance and d isappearance of variability at the orbital period in the power spectrum of the data . This be- havior could be explained by a quasi-cyclical evolution of the equator ial outflow of the Be companion star, whose features influence the conditions for generating gamma rays. These findings open the possibility to use γ -ray observations to study the outflows of massive stars in eccentric binary systems.< Réduire

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Associating long-term γ-ray variability with the superorbital period of LS I + 61◦ 303

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