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Deuterium and Cometary Reservoirs

Introduction: One piece of evidence which may allow us to differentiate between different models of planet formation relates to comets. These icy bodies are likely to retain the isotopic composition they acquired when they formed [1]. As such, it may be possible to determine, from their observed properties, their formation region. Within our Solar system, there are two main reservoirs for these cometary bodies the EdgeworthKuiper belt/Scattered disk and the Oort cloud. It is quite possible that the comets which make up these reservoirs formed in different regions within the planetary nebula, and therefore comets from these different regions may have different compositions. Using a deuterium-enrichment profile, which offers a relationship between the deuterium to hydrogen (henceforth D:H) ratio incorporated in the water within planetesimals and their formation location in the Solar nebula [1] [2] [3] [4], we examine the possible effect that formation in different regions could have on the values of this ratio observed in comets today. We illustrate how such a model, when combined with observations, can lead to conclusions on the regions in which different cometary populations were born.