Suzaku Studies of White Dwarf Stars and the Galactic X-ray Background Emission

  • Takayuki Yuasa
Part of the Springer Theses book series (Springer Theses)

Table of contents

  1. Front Matter
    Pages i-xv
  2. Takayuki Yuasa
    Pages 1-5
  3. Takayuki Yuasa
    Pages 47-59
  4. Takayuki Yuasa
    Pages 89-137
  5. Takayuki Yuasa
    Pages 139-140
  6. Back Matter
    Pages 141-154

About this book

Introduction

This thesis presents a study of the origin of an apparently extended X-ray emission associated with the Galactic ridge. The study was carried out with broadband spectra obtained from mapping observations in the Galactic bulge region conducted in 2005–2010 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. 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. 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.

Keywords

Accretion Column Fe Line from Shock-heated Plasma Galactic Ridge X-ray Emission (GRXE) Intermediate Polar Magnetic White Dwarf Binary Post Shock Region Prize Winning Thesis White Dwarf Star

Authors and affiliations

  • Takayuki Yuasa
    • 1
  1. 1., Department of PhysicsThe University of TokyoTokyoJapan

Bibliographic information

  • DOI https://doi.org/10.1007/978-4-431-54219-3
  • Copyright Information Springer Japan 2013
  • Publisher Name Springer, Tokyo
  • eBook Packages Physics and Astronomy
  • Print ISBN 978-4-431-54218-6
  • Online ISBN 978-4-431-54219-3
  • Series Print ISSN 2190-5053
  • Series Online ISSN 2190-5061
  • About this book