منابع مشابه
The peak radio emission phase variations in the Be - star / X - ray source LSI + 61 ◦ 303
The orbital phase of the peak radio emission in the Be star/X-ray source LSI +61◦ 303 shows variations ranging from 0.5 to 0.9, the weaker emissions showing the larger phase. The delay in attaining peak emission is explained as due to the time required for the relativistic gas bubble responsible for the radio emission, expanding in the hot wind of the Be star, to become large enough in size to ...
متن کاملOptical and infrared modulation in the Be - star / X - ray source LSI + 61 ◦ 303
The Be star X-ray source LSI+61◦303 is found to show optical and infrared modulation with its orbital period. We show that this modulation is due to radiation from a shock produced by the companion to the Be star, while it passes through the gas envelope of the Be star in its binary motion.
متن کاملInverse Compton e ± pair cascade model for the gamma - ray production in massive binary LSI + 61 o 303
We apply an inverse Compton e ± pair cascade model for γ-ray production in the massive binary system LSI +61 o 303 assuming that electrons are accelerated already inside the inner part of the jet launched by the compact object. γ-ray spectra, affected by the cascade process, and lower energy spectra, from the synchrotron cooling of the highest energy electrons in the jet, are calculated as a fu...
متن کاملRapid expansion in the VLBI structure of LSI + 61 ◦ 303
We present the results of global VLBI observations at 6 cm wavelength of the X-ray binary LSI+61◦303 made at epoch 1992.4. During the course of our 24 hour VLBI observing session, the integrated flux measured simultaneously with the VLA indicated that the source was experiencing a minor flare, with the total flux rising and falling by ∼ 12 mJy. Our VLBI observations indicate that this brighteni...
متن کاملThe distances to the X - ray binaries LSI + 61 ◦ 303 and A 0535 + 262
Chevalier & Ilovaisky (1998) use Hipparcos data to show that the X-ray binary systems LSI+61◦ 303 and A0535+262 are a factor of ten closer (i.e. d ∼ few hundred pc) than previously thought (d ∼ 2kpc). We present high quality CCD spectra of the systems, and conclude that the spectral types, reddening and absolute magnitudes of these objects are strongly inconsistent with the closer distances. We...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2004
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20031545