Investigation of High-Mass X-ray binaries
X-ray astronomy, as a branch of astronomy, concentrates on the emission of X-ray of celestial bodies characterized by wavelengths ranging from 0.001 to 100 Å. The first X-ray satellites which have significantly contributed to the development of X-ray astronomy are: Uhuru, Einstein, Röntgensatellit (ROSAT), Advanced Satellite for Cosmology and Astrophysics (ASCA), Rossi X-ray Timing Explorer (RXTE), BeppoSAX, Chandra, and X-ray Multi-Mirror-Newton (XXM-Newton). Generally, an X-ray binary is the brightest source of X-ray emission in the universe, which is composed of a compact star (such as a white dwarf, neutron star, or black hole) and component star (a brown dwarf or white dwarf).
An important focus within X-ray astronomy involves the investigation of high-mass X-ray binaries (HMXBs). A high-mass X-ray binary (HMXB) is defined as a binary system that consists of a massive star and an accreting neutron star or a black hole. In this presentation, I will discuss the formation and evolution of HMXBs, as well as the observation and classification of X-ray binaries.