NATURE OF LOCALIZED POND DEPOSITS ON ASTEROID VESTA
Based on the flow-like surface features of the surrounding region, elevation heterogeneity and eroded topographic conditions of host craters, we hypothesis the downslope transportation of impact/ejecta melts from Marcia and Calpurnia to the topographic lows of the type 1 host craters. We name the smooth lens-like ponds as ejecta ponds. For type 2 pond deposits, we suspected either the low-amplitude seismic frequency and/or subsurface volatile outgassing as a potential carrier to transfer the dust-like granular media. Given the large size of Vesta, we indicate that the localized seismic shaking might be adequate to transport the material downslope. Additionally, Vesta has shown the presence of localized volatile induced surface activities (such as pits, gullies), thus we cannot rule out the subsurface volatile outgassing as a potential event to bring fine and coarse grains from beneath and resettle them on the surface. Nevertheless, both the occasions might be relatively short-lived which do not allow newly accumulated granular material to experience segregation and do not lead to attain smooth surface impression. Since type 2 deposits consist of loose fragmented dusty regolith particles, we name them as dust ponds.
References:  Fujiwara et al., 2006, Science. 312,1330;  Robinson et al., 2001, MPS. 37, 1651-1684;  Plescia and Cintala, 2012, JGR: Planets, 117