  Context: Some apparently quiescent supermassive black holes (BHs) at centers
of galaxies show quasi-periodic eruptions (QPEs) in the X-ray band, the nature
of which is still unknown. A possible origin for the eruptions is an accretion
disk, however the properties of such disks are restricted by the timescales of
reccurance and durations of the flares. Aims: In this work we test the
possibility that the known QPEs can be explained by accretion from a compact
accretion disk with an outer radius $r_{\rm out}\sim 10-40 r_{\rm g}$, focusing
on a particular object GSN 069. Methods: We run several 3D GRMHD simulations
with the {\tt HARMPI} code of thin and thick disks and study how the initial
disk parameters such as thickness, magnetic field configuration, magnetization
and Kerr parameter affect the observational properties of QPEs. Results: We
show that accretion onto a slowly rotating BH through a small, thick accretion
disk with an initially low plasma $\beta$ can explain the observed flare
duration, the time between outbursts and the lack of evidence for a variable
jet emission. In order to form such a disk the accreting matter should have a
low net angular momentum. A potential source for such low angular momentum
matter with a quasi periodic feeding mechanism might be a tight binary of wind
launching stars.
