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Holes and clumps in the interstellar gas of dwarf irregular galaxies aregravitational scattering centers that heat field stars and change their radialand vertical distributions. Because the gas structures are extended and eachstellar scattering is relatively weak, the stellar orbits remain nearlycircular and the net effect accumulates slowly over time. We calculate theradial profile of scattered stars with an idealized model and find that itapproaches an equilibrium shape that is exponential, similar to the observedshapes of galaxy discs. Our models treat only scattering and have no bars orspiral arms, so the results apply mostly to dwarf irregular galaxies wherethere are no other obvious scattering processes. Stellar scattering by gaseousperturbations slows down when the stellar population gets thicker than the gaslayer. An accreting galaxy with a growing thin gas layer can form multiplestellar exponential profiles from the inside-out, preserving the remnants ofeach Gyr interval in a sequence of ever-lengthening and thinning stellarsubdiscs.

Exponential profiles from stellar scattering off interstellar clumps and holes in dwarf galaxy discs