Physics
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agusm.p31c..01m&link_type=abstract
American Geophysical Union, Spring Meeting 2009, abstract #P31C-01
Physics
5422 Ices, 5455 Origin And Evolution, 6224 Kuiper Belt Objects, 6270 Pluto And Satellites, 6285 Trans-Neptunian Objects
Scientific paper
Dwarf planets should form whenever the surface density of a protoplanetary disk is low enough, and as a transient stage during planet formation in more massive disks. In terms of physical attributes (hydrostatic shape, presence of atmospheres, internal oceans, active geology, satellites) there is no clear dividing line bewteen dwarf planets and larger, "regular" planets. In our Solar System, all presently recognized dwarf planets (Eris, Pluto, Haumea, Makemake, Ceres) and former dwarf planets (Triton) are icy, although whether Ceres is a differentiated ice-rich body or a somewhat porous, hydrated rocky body can be debated. Regardless, it is only a matter of time (and data) before the dwarf planets outnumber the 8 "classical" planets. In this talk I will review the question of dwarf planet composition in the Kuiper Belt, including the key role of the solar C/O ratio, the evidence for differentiation (rock core formation) and compositional diversity among these bodies, and the possibility for active cryovolcanism such as may be observed by the New Horizons mission when it reaches the Pluto system in 2015.
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