303 and Psr B1259-63

نویسنده

  • Guillaume Dubus
چکیده

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 as due to γγ absorption and/or changes in shock location along the orbit. Resolved radio emission is due to cooling particles trailing the pulsar. 1 The observational backdrop Thanks to the new generation of Cherenkov telescopes HESS and MAGIC, the past two years have seen a spectacular increase in the number of known sources emitting photons with energies greater than a TeV (see the contributions by Cui, Santangelo and Teshima in this volume). There are now about 40 TeV sources, mostly concentrated in the Galactic plane. Three of the Galactic sources have been associated with binary stars on the basis of their positional coincidence, variability and spectra: PSR B1259-63 (Aharonian et al., 2005b), LS 5039 (Aharonian et al., 2005a) and LS I +61303 (Albert et al., 2006).

برای دانلود متن کامل این مقاله و بیش از 32 میلیون مقاله دیگر ابتدا ثبت نام کنید

ثبت نام

اگر عضو سایت هستید لطفا وارد حساب کاربری خود شوید

منابع مشابه

X-ray emission from the PSR B1259–63 system near apastron

The PSR B1259–63 system contains a 47 ms radio pulsar in a highly eccentric binary with a Be-star companion. Strongly time variable X-ray emission was reported from this system as the pulsar was near apastron in 1992-early 1993. The variability was primarily deduced from an apparent non-detection of the PSR B1259-63 system during a first pre-apastron ROSAT observation in February 1992. We have ...

متن کامل

Suzaku Observations of Psr B1259−63: a New Manifestation of Relativistic Pulsar Wind

We observed PSR B1259−63, a young non-accreting pulsar orbiting around a Be star SS 2883, eight times with the Suzaku satellite from July to September 2007, to characterize the X-ray emission arising from the interaction between a pulsar relativistic wind and Be star outflows. The X-ray spectra showed a featureless continuum in 0.6–10 keV, modeled by a power law with a wide range of photon inde...

متن کامل

X-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 کامل

X-Ray/Gamma-Ray Observations of the PSR B1259−63/SS 2883 system near Apastron

We report the results from X-ray and hard X-ray observations of the PSR B1259−63/SS 2883 system with the ASCA and CGRO satellites, performed between 1995 February and 1996 January when the pulsar was near apastron. The system was clearly detected in each of the two ASCA observations with luminosity in the 1–10 keV band of LX = (9 ± 3) × 10 32 (d/2 kpc) erg s, while CGRO/OSSE did not detect sign...

متن کامل

Diffractive 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 کامل

ذخیره در منابع من


  با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید

برای دانلود متن کامل این مقاله و بیش از 32 میلیون مقاله دیگر ابتدا ثبت نام کنید

ثبت نام

اگر عضو سایت هستید لطفا وارد حساب کاربری خود شوید

عنوان ژورنال:

دوره   شماره 

صفحات  -

تاریخ انتشار 2006