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The study was carried out with broadband spectra obtained from mapping observations in the Galactic bulge region conducted in — by the Suzaku space X-ray observatory. The spectra were analyzed with a newly constructed X-ray spectral model of an accreting white dwarf binary that is one of the proposed candidate stars for the origin of the Galactic ridge emission in the higher energy band. The result, together with previously reported high-resolution imaging results, strongly supports the idea that the Galactic ridge X-ray emission is an assembly of dim, discrete X-ray point sources. The study was carried out with broadband spectra Fitting of the observed Galactic ridge spectra with the model showed that there is another spectral component that fills the gap between the observed X-ray flux and the component expected from the accreting white dwarf spectral model in the lower energy band. This thesis presents a study of the origin of an apparently extended X-ray emission associated with the Galactic ridge.

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This thesis presents a study of the origin of an apparently extended X-ray emission associated with the Galactic ridge. The spectra were analyzed with a newly constructed X-ray spectral model of an accreting white dwarf binary that is one of the proposed candidate stars for the origin of the Galactic ridge emission in the higher energy band. The study was carried out with broadband spectra The result, together with previously reported high-resolution imaging results, strongly supports the idea that the Galactic ridge X-ray emission is an assembly of dim, discrete X-ray point sources. This additional soft spectral component was nicely explained by an X-ray spectral model of normal stars. The study was carried out with broadband spectra obtained from mapping observations in the Galactic bulge region conducted in — by the Suzaku space X-ray observatory. Fitting of the observed Galactic ridge spectra with the model showed that there is another spectral component that fills the gap between the observed X-ray flux and the component expected from the accreting white dwarf spectral model in the lower energy band. The spectra were analyzed with a newly constructed X-ray spectral model of an accreting white dwarf binary that is one of the proposed candidate stars for the origin of the Galactic ridge emission in the higher energy band. The result, together with previously reported high-resolution imaging results, strongly supports the idea that the Galactic ridge X-ray emission is an assembly of dim, discrete X-ray point sources. The study was carried out with broadband spectra obtained from mapping observations in the Galactic bulge region conducted in — by the Suzaku space X-ray observatory. The study was carried out with broadband spectra This thesis presents a study of the origin of an apparently extended X-ray emission associated with the Galactic ridge. Fitting of the observed Galactic ridge spectra with the model showed that there is another spectral component that fills the gap between the observed X-ray flux and the component expected from the accreting white dwarf spectral model in the lower energy band. This additional soft spectral component was nicely explained by an X-ray spectral model of normal stars.

 

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