منابع مشابه
303 and Psr B1259-63
Three binaries are now established sources of emission at very high energies (>10 eV). They are composed of a massive star and a compact object. The emission can be due to the interaction of the relativistic wind from a young ms pulsar with the stellar wind of the companion (Maraschi & Treves, 1981), by which rotation-power ends up as non-thermal flux. Variations at VHE energies are explained a...
متن کاملDiffractive Scintillation of the Pulsar PSR B1259-63
PSR B1259–63 is in a highly eccentric 3.4 yr orbit around the Be-star SS2883. The system is located in the direction of the Sagittarius-Carina spiral arm at a distance of ∼1.5 kpc. We have made scintillation observations of the pulsar far from periastron at 4.8 GHz and 8.4 GHz, determining the diffractive bandwidth, ∆νd, and timescale, ∆td, at both frequencies. We find no dependency on orbital ...
متن کاملX-ray Detection of Psr B1259?63 at Periastron
We report on results of X-ray observations of the unique radio pulsar/Be star binary PSR B1259?63, obtained using the ASCA satellite two weeks before, during , and two weeks after the pulsar's most recent periastron passage on January 9, 1994. The source was detected at all three epochs, with an X-ray luminosity in the 1{10 keV band of 110 34 (d=2 kpc) 2 erg s ?1 at the pre-and post-periastron ...
متن کاملTiming of the Binary Pulsar PSR B1259−63
Timing of PSR B1259−63, the first radio pulsar discovered to have a massive main-sequence companion, has been carried out since 1990. The timing is complicated because the orbital period is very long, the pulsar is eclipsed for 40 days around periastron, the pulsar has significant timing noise and also has been seen to glitch. A model for the timing data based on spin-orbit coupling no longer p...
متن کاملHydrodynamic Interaction between the Be Star and the Pulsar in the TeV Binary PSR B1259 63/LS 2883
We have been studying the interaction between the Be star and the pulsar in the TeV binary PSR B1259 63/LS 2883, using 3-D SPH simulations of the tidal and wind interactions in this Be–pulsar system. We first ran a simulation without pulsar wind nor Be wind, while taking into account only the gravitational effect of the pulsar on the Be disk. In this simulation, the gas particles are ejected at...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2007
ISSN: 0035-8711,1365-2966
DOI: 10.1111/j.1365-2966.2007.12075.x