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The formation of brown dwarfs via encounters between proto-stars has beenconfirmed with high-resolution numerical simulations with a restrictedtreatment of the thermal conditions. The new results indicate that young browndwarfs (BDs) formed this way are disk-like and often reside in multiplesystems. The newly-formed proto-BDs disks are up to 18 AU in size and spinrapidly making small-scale bipolar outflows, fragmentation and the possibleformation of planetary companions likely as have recently been observed forBDs. The object masses range from 2 to 73 Jupiter masses, distributed in amanner consistent with the observed sub-stellar initial mass function. Thesimulations usually form multiple BDs on eccentric orbits about a star. Onesuch system was hierarchical, a BD binary in orbit around a star, which mayexplain recently observed hierarchical systems. One third of the BDs wereunbound after a few thousand years and interactions among orbiting BDs mayeject more or add to the number of binaries. Improvements over prior workinclude resolution down to a Jupiter mass, self-consistent models of thevertical structure of the initial disks and careful attention to avoidartificial fragmentation.Comment: 4 pages, 3 figures, accepted for publication in ApJ Letter

Proto-Brown Dwarf Disks as Products of Protostellar Disk Encounters