AGGREGATION OF SiC-X GRAINS IN SUPERNOVA EJECTA

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dc.contributor.authorDeneault, Ethan A.-N.
dc.date.accessioned2018-10-05T14:31:47Z
dc.date.available2018-10-05T14:31:47Z
dc.date.copyright© 2009. The American Astronomical Society. All rights reserved
dc.date.issued2009-10-20
dc.description© 2009. The American Astronomical Society. All rights reserved
dc.descriptionFinal Published Version
dc.description.abstractWe present a model for the formation of silicon carbide aggregates within the expanding and cooling supernova remnant. SiC type-X (SiC-X) grains measured in the laboratory at a high spatial resolution have been found to be aggregates of smaller crystals which are isotopically homogenous. The initial condensation of SiC in the ejecta occurs within an interior dense shell of material which is created by a reverse shock which rebounds from the core–envelope interface. A subsequent reverse shock accelerates the grains forward, but the gas drag from the ejecta on the rapidly moving particles limits their travel distance. By observing the effects of gas drag on the travel distance of grains, we propose that supernova grain aggregates form from material that condensed in a highly localized region, which satisfies the observational evidence of isotopic homogeneity in SiC-X grains.en_US
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dc.identifier.citationAGGREGATION OF SiC-X GRAINS IN SUPERNOVA EJECTA 2009, 705: 1215-1218 TheAstrophysical Journalen_US
dc.identifier.doihttps://doi.org/10.1088/0004-637X/705/2/1215
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/20.500.11868/569
dc.language.isoen_USen_US
dc.publisherThe American Astronomical Societyen_US
dc.rights© 2009. The American Astronomical Society. All rights reserved.
dc.source.urihttp://iopscience.iop.org/article/10.1088/0004-637X/705/2/1215
dc.subjectSupernova remnants – infrareden_US
dc.subjectStars – astrochemistryen_US
dc.titleAGGREGATION OF SiC-X GRAINS IN SUPERNOVA EJECTAen_US
dc.typeArticleen_US

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2009 CNHS Faculty Publications