• DOI:10.1111/J.1365-2966.2009.15116.X
• Corpus ID: 122635141

X-ray observations of PSR B1259−63 near the 2007 periastron passage

@article{Chernyakova2009XrayOO,
  title={X-ray observations of PSR B1259−63 near the 2007 periastron passage},
  author={M Chernyakova and Andrii Neronov and Felix Aharonian and Yasunobu Uchiyama and Tadayuki Takahashi},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2009},
  volume={397},
  pages={2123-2132}
}

• M. Chernyakova, A. Neronov, +2 authors Tadayuki Takahashi
• Published 21 August 2009
• Physics
• Monthly Notices of the Royal Astronomical Society

PSR B1259‐63 is a 48 ms radio pulsar in a highly eccentric 3.4 year orbit with a Be star SS 2883. Unpulsedγ-ray, X-ray and radio emission components are observed from the binary system. It is likely that the collision of the pulsar wind wit h the anisotropic wind of the Be star plays a crucial role in the generation of the observed no n-thermal emission. The 2007 periastron passage was observed in unprecedented details with Suzaku, Swift, XMM-Newton and Chandra missions. We present here the results of this campaign and compare them with previous observations. With these data we are able, for the fi rst time, to study the details of the spectral evolution of the source over a 2 months period of the passage of the pulsar close to the Be star. New data confirm the pre-periastron spectral h ardening, with the photon index reaching a value smaller than 1.5, observed during a local flu x minimum. If the observed X-ray emission is due to the inverse Compton (IC) losses of the 10 MeV electrons, then such a hard spectrum can be a result of Coulomb losses, or can be related to the existence of the low-energy cut-off in the electron spectrum. Alternatively, if the X-ray emiss ion is a synchrotron emission of very high energy electrons, the observed hard spectrum can be explained if the high energy electrons are cooled by IC emission in Klein-Nishina regime. Unfortunately the lack of simultaneous data in the TeV energy band prevents us from making a definite conclusion on the nature of the observed spectral h ardening and, therefore, on the origin of the X-ray emission.