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Milky Way X-ray background emission
« »: , . «» , 30- . . We all know that the name our position at the edge of the X-ray band the analog origin of this X-ray emissio "Milky Way" of our Galaxy stands for special appearance which it has when we look at it from the Galaxy: large number of stars in the Galactic plane form a glowing stripe across the sky. In of the "Milky Way" is a Galactic ridge, which was discovered more than 30 years ago. The n was a mystery for astronomers for more than 30 years.

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Resent studies of Galactic X-ray background by efforts of Russian scientists (IKI RAN, Moscow) allow to solve long-aged mystery. Using near-infrared Galaxy intensity measured with COBE/DIRBE experiment and X-ray data from RXTE and INTEGRAL it was shown that X-ray brightness of the Galactic background emission closely follows its stellar density and can be explained by a cumulative emission of a large number of weak Galactic X-ray sources.

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In hard X-rays, which has become available for study with the INTEGRAL observatory, the Ridge emission is made of accreting white dwarf binaries.

17-60 keV

. . Map of Galactic background emission in hard X-ray energy band obtained with INTEGRAL observatory. Green contours represent near-infrared brightness of Galaxy.

, 3100 ( ). RXTE . .
Galactic background emission in 3-100 keV energy band originates as a sum of emission of coronally active stars and cataclysmic variables. Spectrum of background is shown on the right (RXTE+INTEGRAL).

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In accreting white dwarfs X-ray photons originate in very hot (up to hundred of million degrees) plasma, heated up in the shock standing above the surface of the white dwarf, which transfer kinetic energy of the matter falling with the velocities ~1000 km/sec into heat. INTEGRAL data allows to estimate the average mass of accreting white dwarfs in the Galaxy

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