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Numerical modelling of gas flows in galaxy centres

Recent observations of the central parts of galaxies reveal an ever-improving view of the complex structures residing therein: rings, spirals and gas flows, often feeding the central supermassive black holes. The James Webb Space Telescope should increase the available data significantly, but its interpretation requires detailed numerical simulations. During the course of the PhD, the student will create and develop a model explaining the accretion of matter on to a black hole in a realistic environment of the central parts of a galaxy, on spatial scales from the size of the accretion disc to ~10 parsecs. The obtained results will help understand how black hole accretion rates change on timescales of a million years and connect the structures observed in galaxy centres to the activity episodes of those galaxies. Such a model will also fill the gap between detailed simulations of accretion disc evolution and large-scale galaxy evolution simulations.
 
For more information, please contact the theme supervisor K. Zubovas.