Cover credits: NASA and the Chandra X-ray Center (CXC).
CONTENTS v
BibliographyNederlandse samenvatting Acknowledgments 2 chapter 1: Introduction
Low Mass X-ray BinariesLow mass X-ray binaries (LMXBs) are among the brightest sources in the Xray sky when they are actively accreting. In an LMXB, the companion is a star of mass less than that of the Sun. The accretion process is powered from the Roche-lobe overflow in which case the material from the companion star accretes via the gravitational equilibrium position to the compact object. In this case, a stable accretion disk can form (Shakura & Sunyaev 1973). The optical emission from the companion star in LMXBs is detectable, which is much fainter than the X-ray emission.As of now, around 200 LMXBs, confirmed and potential, have been identified in our Galaxy primarily through both their X-ray and optical properties (Liu, van Paradijs & van den Heuvel 2007;Tetarenko et al. 2016;Corral-Santana et al. 2016). While the nature of the compact object in many LMXBs is still unknown, for tens of systems we have identified whether they contain black holes or neutron stars (NSs). Among the ∼ 200 LMXBs, approximately 70 are BH LMXBs, while the number of known NS-LMXBs is approximately twice that of BH-LMXBs, consistent with theoretical predictions based on the formation history of NSs and BHs (Kalogera & Webbink 1998).1.2: X-ray Components of Black Hole X-ray Binaries * For X-ray binary in the soft state (see 1.3 for more details), the thermal component can be readily observed in the X-ray band, while for Active Galactic Nuclei (AGN), the thermal component appears in the UV/optical band.