Multiwavelength observations of the binary system PSR B1259-63/LS 2883 around the 2010-2011 periastron passage

M. Chernyakova (1, 2) , A.A. Abdo (3) , A. Neronov (4) , M.V. Mcswain (5) , J. Moldón (6, 7) , M. Ribó (6) , J.M. Paredes (6) , I. Sushch (8, 9, 10) , M. de Naurois (11) , U. Schwanke (10) , Y. Uchiyama (12, 13) , K. Wood (14) , S. Johnston (15) , S. Chaty (16, 17) , A. Coleiro (16) , D. Malyshev (4, 18) , I. Babyk (1, 2)

1 DCU - Dublin City University [Dublin]
2 DIAS - Dublin Institute for Advanced Studies
3 Operational Evaluation Division, Institute for Defense Analyses, 4850 Mark Center Drive Alexandria, VA 22311-1882, United States
4 INTEGRAL Science Data Center, Chemin d'écogia 16, 1290 Versoix, Switzerland
5 Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem PA 18015, United States
6 Departament d'Astronomia i Meteorologia [Barcelona]
7 ASTRON - Netherlands Institute for Radio Astronomy
8 Centre for Space Research [Potchefstroom]
9 Astronomical Observatory of Ivan Franko National University of L'viv
10 HU Berlin - Humboldt-Universität zu Berlin = Humboldt University of Berlin = Université Humboldt de Berlin
11 LLR - Laboratoire Leprince-Ringuet
12 SLAC National Accelerator Laborat 2575 Sand Hill Road, Menlo Park, CA 94025, United States
13 Department of Physics [Tokyo]
14 U.S. Naval Research Lab 4555 Overlook Ave., SW Washington DC 20375, United States
15 CSIRO Astronomy and Space Science
16 AIM (UMR7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
17 IUF - Institut universitaire de France
18 Bogolyubov Institute for Theoretical Physics

We report on broad multiwavelength observations of the 2010-2011 periastron passage of the ?-ray loud binary system PSR B1259-63. High-resolution interferometric radio observations establish extended radio emission trailing the position of the pulsar. Observations with the Fermi Gamma-ray Space Telescope reveal GeV ?-ray flaring activity of the system, reaching the spin-down luminosity of the pulsar, around 30d after periastron. There are no clear signatures of variability at radio, X-ray and TeV energies at the time of the GeV flare. Variability around periastron in the Ha emission line, can be interpreted as the gravitational interaction between the pulsar and the circumstellar disc. The equivalent width of the Ha grows from a few days before periastron until a few days later, and decreases again between 18 and 46 d after periastron. In near-infrared we observe the similar decrease of the equivalent width of Br? line between the 40th and 117th day after the periastron. For the idealized disc, the variability of the Ha line represents the variability of the mass and size of the disc. We discuss possible physical relations between the state of the disc and GeV emission under assumption that GeV flare is directly related to the decrease of the disc size. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Domaines: Physique [physics]; Planète et Univers [physics]

M. Chernyakova, A.A. Abdo, A. Neronov, M.V. Mcswain, J. Moldón, et al.. Multiwavelength observations of the binary system PSR B1259-63/LS 2883 around the 2010-2011 periastron passage. Monthly Notices of the Royal Astronomical Society, 2014, 439 (1), pp.432-445. ⟨10.1093/mnras/stu021⟩. ⟨hal-01087272⟩