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Modelling of Comptonisation in low-mass X-ray binaries in the presence of fast variability

PhD ceremony:Mr K. (Kostas) Karpouzas
When:November 19, 2021
Supervisors:prof. dr. R.M. (Mariano) Mendez, prof. dr. D. Altamirano
Where:Academy building RUG
Faculty:Science and Engineering
Modelling of Comptonisation in low-mass X-ray binaries in the
presence of fast variability

Comptonisation is a physical phenomenon that describes how radiation emitted from a source changes while travelling through a medium. In low-mass X-ray binaries (LMXBs) a compact object, which is a neutron star (NS) or a black-hole (BH), emits X-ray radiation that passes through a medium, called the corona. The corona is in a sense the atmosphere of an LMXB. After passing through the corona, the radiation that reaches our telescopes is observed to oscillate on time-scales of micro-seconds to a few seconds.

In this thesis I have developed a mathematical model that explains both the radiation profile received by telescopes and also how that radiation, at different wavelengths, is oscillating as a function of time. By comparing the predictions of the model to real observations, we have concluded that: (a) The LMXBs that contain a neutron star are likely to have a corona that is around a hundred times smaller and 10 times more dense than that of LMXBs containing a black-hole, (b) the size of the corona of BH LMXBs changes reccurently between very large and very small leading to a different interaction between the corona and matter around the BH and (c) the corona around BH LMXBs can be ejected, with the help of magnetic fields, forming the so-called jet and later re-appear in its previous form. Our results have provided, for the first time, quantitative evidence for phenomena that were suggested in the literature decades ago.