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- W89839323 abstract "9 I. HISTORY o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o o Recent gr und-based bservati ns have unveiled a large number f b dies in rbit bey nd Neptune, in a regi n n w widely kn wn as the Kuiper ( r, less c mm nly, Edgew rth-Kuiper) Belt. Ab ut 10 Kuiper Belt bjects (KBOs) with diameters larger than 100 km exist in the 30-AU t 50-AU trans-Neptunian regi n. Their c mbined mass is ab ut 10% f that f Earth. The rbits f KBOs fall int at least three distinct dynamical classes: the “Classical” bjects, the Plutin s, and the “Scattered” bjects. Each thr ws light n physical pr cesses perating in the s lar system pri r t and during the f rmati n f the planets. The Kuiper Belt is significant b th as the likely s urce f the sh rt-peri d c mets (and the dynamically intermediate Centaurs) and as a rep sit ry f the s lar system’s m st primitive (least thermally pr cessed) material. KBOs sh w an unexpected and presently unexplained diversity f surface c l rs, p ssibly reflecting intrinsic c mp siti nal variati ns and transient resurfacing by impacts. The present-day Kuiper Belt is pr bably the surviving remnant f a nce much m re massive (10 M ?) preplanetary disk. It is very likely that c llisi ns and disk-planet interacti ns played a maj r r le in shaping this early precurs r. Alth ugh the c llisi nal pr ducti n f dust is presently m dest ( 10 kg s ) and the ptical depth small ( 10 ), the early Belt was pr bably very dusty and may have sustained a disk anal g us t th se rep rted ar und s me nearby main-sequence stars." @default.
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- W89839323 date "2000-05-01" @default.
- W89839323 modified "2023-09-23" @default.
- W89839323 title "Physical Nature of the Kuiper Belt" @default.
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