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Haumea, a rapidly rotating elongated dwarf planet (~ 1500 km in diameter),has two satellites and is associated with a "family" of several smaller KuiperBelt objects (KBOs) in similar orbits. All members of the Haumea system share awater ice spectral feature that is distinct from all other KBOs. The relativevelocities between the Haumea family members are too small to have formed bycatastrophic disruption of a large precursor body, which is the process thatformed families around much smaller asteroids in the Main Belt. Here we showthat all of the unusual characteristics of the Haumea system are explained by anovel type of giant collision: a graze-and-merge impact between two comparablysized bodies. The grazing encounter imparted the high angular momentum thatspun off fragments from the icy crust of the elongated merged body. Thefragments became satellites and family members. Giant collision outcomes areextremely sensitive to the impact parameters. Compared to the Main Belt, thelargest bodies in the Kuiper Belt are more massive and experience slowervelocity collisions; hence, outcomes of giant collisions are dramaticallydifferent between the inner and outer solar system. The dwarf planets in theKuiper Belt record an unexpectedly large number of giant collisions, requiringa special dynamical event at the end of solar system formation.

The Formation of the Collisional Family around the Dwarf Planet Haumea