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Following the Interstellar History of Carbon: From the Interiors of Stars to the Surfaces of Planets
Stockholm University, Faculty of Science, Department of Physics.
Number of Authors: 4
2016 (English)In: Astrobiology, ISSN 1531-1074, E-ISSN 1557-8070, Vol. 16, no 12, 997-1012 p.Article in journal (Refereed) Published
Abstract [en]

The chemical history of carbon is traced from its origin in stellar nucleosynthesis to its delivery to planet surfaces. The molecular carriers of this element are examined at each stage in the cycling of interstellar organic material and their eventual incorporation into solar system bodies. The connection between the various interstellar carbon reservoirs is also examined. Carbon has two stellar sources: supernova explosions and mass loss from evolved stars. In the latter case, the carbon is dredged up from the interior and then ejected into a circumstellar envelope, where a rich and unusual C-based chemistry occurs. This molecular material is eventually released into the general interstellar medium through planetary nebulae. It is first incorporated into diffuse clouds, where carbon is found in polyatomic molecules such as H2CO, HCN, HNC, c-C3H2, and even C-60(+). These objects then collapse into dense clouds, the sites of star and planet formation. Such clouds foster an active organic chemistry, producing compounds with a wide range of functional groups with both gas-phase and surface mechanisms. As stars and planets form, the chemical composition is altered by increasing stellar radiation, as well as possibly by reactions in the presolar nebula. Some molecular, carbon-rich material remains pristine, however, encapsulated in comets, meteorites, and interplanetary dust particles, and is delivered to planet surfaces.

Place, publisher, year, edition, pages
2016. Vol. 16, no 12, 997-1012 p.
Keyword [en]
Carbon isotopes, Prebiotic evolution, Interstellar molecules, Comets, Meteorites
National Category
Physical Sciences Biological Sciences Earth and Related Environmental Sciences
Identifiers
URN: urn:nbn:se:su:diva-140264DOI: 10.1089/ast.2016.1484ISI: 000391853800007PubMedID: 28001448OAI: oai:DiVA.org:su-140264DiVA: diva2:1081975
Available from: 2017-03-15 Created: 2017-03-15 Last updated: 2017-03-15Bibliographically approved

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CiteExportLink to record
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Citation style
  • apa
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