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  • American Association for the Advancement of Science (AAAS)  (2)
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  • 1
    Publication Date: 2014-09-27
    Description: Identifying the source of Earth's water is central to understanding the origins of life-fostering environments and to assessing the prevalence of such environments in space. Water throughout the solar system exhibits deuterium-to-hydrogen enrichments, a fossil relic of low-temperature, ion-derived chemistry within either (i) the parent molecular cloud or (ii) the solar nebula protoplanetary disk. Using a comprehensive treatment of disk ionization, we find that ion-driven deuterium pathways are inefficient, which curtails the disk's deuterated water formation and its viability as the sole source for the solar system's water. This finding implies that, if the solar system's formation was typical, abundant interstellar ices are available to all nascent planetary systems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Cleeves, L Ilsedore -- Bergin, Edwin A -- Alexander, Conel M O'D -- Du, Fujun -- Graninger, Dawn -- Oberg, Karin I -- Harries, Tim J -- New York, N.Y. -- Science. 2014 Sep 26;345(6204):1590-3. doi: 10.1126/science.1258055.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of Michigan, 311 West Hall, 1085 South University Avenue, Ann Arbor, MI 48109, USA. cleeves@umich.edu. ; Department of Astronomy, University of Michigan, 311 West Hall, 1085 South University Avenue, Ann Arbor, MI 48109, USA. ; Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA. ; Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 02138, USA. ; Department of Physics and Astronomy, University of Exeter, Stocker Road, Exeter EX4 4QL, UK.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25258075" target="_blank"〉PubMed〈/a〉
    Keywords: Deuterium/chemistry ; Earth (Planet) ; *Ice ; Origin of Life ; *Solar System
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 2
    Publication Date: 2013-07-23
    Description: Planets form in the disks around young stars. Their formation efficiency and composition are intimately linked to the protoplanetary disk locations of "snow lines" of abundant volatiles. We present chemical imaging of the carbon monoxide (CO) snow line in the disk around TW Hya, an analog of the solar nebula, using high spatial and spectral resolution Atacama Large Millimeter/Submillimeter Array observations of diazenylium (N2H(+)), a reactive ion present in large abundance only where CO is frozen out. The N2H(+) emission is distributed in a large ring, with an inner radius that matches CO snow line model predictions. The extracted CO snow line radius of ~30 astronomical units helps to assess models of the formation dynamics of the solar system, when combined with measurements of the bulk composition of planets and comets.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Qi, Chunhua -- Oberg, Karin I -- Wilner, David J -- D'Alessio, Paola -- Bergin, Edwin -- Andrews, Sean M -- Blake, Geoffrey A -- Hogerheijde, Michiel R -- van Dishoeck, Ewine F -- New York, N.Y. -- Science. 2013 Aug 9;341(6146):630-2. doi: 10.1126/science.1239560. Epub 2013 Jul 18.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA. cqi@cfa.harvard.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23868917" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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