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Supermassive black holes reside in cores of galaxies, where they are oftensurrounded by a nuclear cluster and a clumpy torus of gas and dust. Mutualinteractions can set some stars on a plunging trajectory towards the blackhole. We model the pericentre passage of a dust-enshrouded star during whichthe dusty envelope becomes stretched by tidal forces and is affected by theinteraction with the surrounding medium. In particular, we explore under whichconditions these encounters can lead to periods of enhanced accretion activity.We discuss different scenarios for such a dusty source. To this end, weemployed a modification of the Swift integration package. Elements of the cloudwere modelled as numerical particles that represent the dust component thatinteracts with the optically thin gaseous environment. We determine thefraction of the total mass of the dust component that is diverted from theoriginal path during the passages through the pericentre at $\sim 10^3$Schwarzschild radii and find that the main part of the dust ($\gtrsim 90\%$ ofits mass) is significantly affected upon the first crossing. The fraction ofmass captured at the second passage generally decreases to very low values. Asan example, we show predictions for the dusty source evolution assuming thecurrent orbital parameters of the G2 cloud (also known as Dusty S-ClusterObject, DSO) in our Galactic centre. Encounter of a core-less cloud with asupermassive black hole is, most likely, a non-repeating event: the cloud isdestroyed. However, in the case of a dust-enshrouded star, part of the envelopesurvives the pericentre passage. We discuss an offset of $\lesssim 0.3$ arcsecbetween the centre of mass of the diverted part and the star along theeccentric orbit. Finally, we examine an interesting possibility of a binarystar embedded within a common wind envelope that becomes dispersed at thepericentre passage.

Dust-enshrouded star near supermassive black hole: predictions for high-eccentricity passages near low-luminosity galactic nuclei