X-Ray binaries (XRBs) are accreting systems hosting a star and a compact object. Giacconi et al. (1962) serendipitously discovered the first of these sources, i.e. Sco X-1, during an X-ray observation of the Moon. There are three types of compact objects that can take part in a binary system: a white dwarf (WD), a neutron star (NS), or a black hole (BH). If the compact object is either a NS or a WD, it can feature a strong surface magnetic field B~1012-15 Gauss, or B~106 Gauss, respectively. The magnetic field influences the accretion flow, by driving matter to the accreting column. Strong magnetic field in NS, also, imprints the X-ray spectrum emitted by the compact object, in the form of absorption lines, referred to as cyclotron lines. A further distinction is based on the mass (and therefore the spectral type) of the companion star. If the mass of the companion is more than 10 Msun the system is referred to as a High Mass X-ray Binary (HMXB). If the mass of the companion star is less than 1 Msun then it is referred to as a Low Mass X-ray binary (LMXB). Finally, if the mass of the companion falls in between 1 Msun and 10 Msun thenit is referred to as an Intermediate Mass X-ray Binary (IMXB).


My Research Interests can be summarized as follows:

X-ray Binaries


Stellar winds