  Super-puffs -- low-mass exoplanets with extremely low bulk density -- are
attractive targets for exploring their atmospheres and formation processes.
Recent studies suggested that the large radii of super-puffs may be caused by
atmospheric dust entrained in the escaping atmospheres. In this study, we
investigate how the dust grows in escaping atmospheres and influence the
transit radii using a microphysical model of grain growth. Collision growth is
efficient in many cases, leading to hinder the upward transport of dust via
enhanced gravitational settling. We find that dust abundance in the outflow
hardly exceeds the Mach number at the dust production region. Thus, dust formed
at upper atmospheres, say $P\lesssim{10}^{-5}$ bar, are needed to launch a
dusty outflow with high dust abundance. With sufficiently high dust production
altitudes and rates, the dusty outflow can enhance the observable radius by a
factor of $\sim$2 or even more. We suggest that photochemical haze is a
promising candidate of high-altitude dust that can be entrained in the outflow.
We also compute the synthetic transmission spectra of super-puff atmospheres
and demonstrate that the dusty outflow produces a broad spectral slope and
obscures molecular features, in agreement with recently reported featureless
spectra. Lastly, using an interior structure model, we suggest that the
atmospheric dust could drastically enhance the observable radius only for
planets in a narrow mass range of $\sim2$--$5M_{\rm \oplus}$, in which the
boil-off tends to cause total atmospheric loss. This may explain why
super-puffs are uncommon despite the suggested universality of photochemical
hazes.
