Biology
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.7102k&link_type=abstract
American Astronomical Society Meeting 210, #71.02; Bulletin of the American Astronomical Society, Vol. 39, p.178
Biology
Scientific paper
It is generally accepted that a considerable fraction of early Earths
water was delivered by asteroids, comets, and planetesimals. The local
planets and comets were assembled from the material in circumstellar
disks, which in turn evolved from the envelopes and clouds surrounding
protostars. Here at the University of Hawaii-NASA Astrobiology
Institute the key research goal is to connect the major aspects of starformation and planetary water, in effect aiming to understand the terms of a "watery Drake Equation". To achieve this goal, we use the infrared and submillimeter telescopes on Mauna Kea to survey several molecules in a variety of starforming clouds. Observations show that water is the most common interstellar ice component. Moreover, there is evidence for enhanced water ice formation in the inner parts of protostellar envelopes. Simple molecules form on the icy grain mantles from surface reactions or thermal annealing of the ice, in turn these molecules drive a rich gas phase chemistry that produces more complex prebiotic molecules. Ice bands, therefore, serve as unique tracers of the chemical and thermal history of circumstellar environments. Here we will discuss constraints on the reservoirs of water and organic molecules in starforming regions, taking in to account the latest observational and theoretical measurements. Recent observations of a number of deuterated molecules, including water, will be discussed in terms of grain surface chemistry and its role in driving the enhanced fractionation of methanol like species, while at the same time inhibiting the deuteration of water.
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