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The X-ray source HLX-1 near the spiral galaxy ESO 243-49 is currently thebest intermediate-mass black hole candidate. It has a peak bolometricluminosity of $10^{42}$ erg s$^{-1}$, which implies a mass inflow rate of$\sim10^{-4}$ MSun yr$^{-1}$, but the origin of this mass is unknown. It hasbeen proposed that there is a star on an eccentric orbit around the black holewhich transfers mass at pericentre. To investigate the orbital evolution ofthis system, we perform stellar evolution simulations using mesa and SPHsimulations of a stellar orbit around an intermediate-mass black hole using fi.We run and couple these simulations using the amuse framework. We find thatmass is lost through both the first and second Lagrange points and that thereis a delay of up to 10 days between the pericentre passage and the peak massloss event. The orbital evolution timescales we find in our simulations arelarger than what is predicted by analytical models, but these models fallwithin the errors of our results. Despite the fast orbital evolution, we areunable to reproduce the observed change in outburst period. We conclude thatthe change in the stellar orbit with the system parameters investigated here isunable to account for all observed features of HLX-1.

Simulations of the tidal interaction and mass transfer of a star in an eccentric orbit around an intermediate-mass black hole: the case of HLX-1