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Aims: Response of a protoplanetary disk to luminosity bursts of variousduration is studied with the purpose to determine the effect of the bursts onthe strength and sustainability of gravitational instability in the disk. Aspecial emphasis is paid to the spatial distribution of gas and grown dust(from 1 mm to a few cm) during and after the burst. Methods: Numericalhydrodynamics simulations using the FEOSAD code were employed to study thedynamics of gas and dust in the thin-disk limit. Dust-to-gas friction includingback reaction and dust growth were also considered. Bursts of various duration(from 100 to 500 yr) were initiated in accordance with a thermally ignitedmagnetorotational instability. Luminosity curves for constant- anddeclining-magnitude bursts were adopted to represent two typical limiting casesfor FU-Orionis-type eruptions. Results: The short-term effect of the burst isto reduce the strength of gravitational instability by heating and expandingthe disk. The longest bursts with duration comparable to the revolution periodof the spiral can completely dissolve the original two-armed spiral pattern inthe gas disk by the end of the burst, while the shortest bursts only weaken thespiral pattern. The reaction of grown dust to the burst is somewhat different.The spiral-like initial distribution with deep cavities in the inter-armedregions transforms into a ring-like distribution with deep gaps. Thistransformation is most expressed for the longest-duration bursts. The long-termeffect of the burst depends on the initial disk conditions at the onset of theburst. In some cases, vigorous disk fragmentation sets in several thousandyears after the burst, which was absent in the model without the bursts(abridged).

The effect of luminosity outbursts on the protoplanetary disk dynamics