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dc.contributor.authorHaenecour, Pierre
dc.contributor.authorHowe, Jane Y.
dc.contributor.authorZega, Thomas J.
dc.contributor.authorAmari, Sachiko
dc.contributor.authorLodders, Katharina
dc.contributor.authorJosé Pont, Jordi
dc.contributor.authorKaji, Kazutoshi
dc.contributor.authorSunaoshi, Takeshi
dc.contributor.authorAtsushi, Muto
dc.contributor.otherUniversitat Politècnica de Catalunya. Departament de Física
dc.date.accessioned2019-06-05T13:08:27Z
dc.date.available2019-06-05T13:08:27Z
dc.date.issued2019-04-29
dc.identifier.citationHaenecour, P. [et al.]. Laboratory evidence for co-condensed oxygen- and carbon-rich meteoritic stardust from nova outbursts. "Nature Astronomy", 29 April 2019, No 3, pp. 626-630
dc.identifier.issn2397-3366
dc.identifier.urihttp://hdl.handle.net/2117/134009
dc.description.abstractAlthough their parent stars no longer exist, the isotopic and chemical compositions and microstructure of individual stardust grains identified in meteorites provide unique constraints on dust formation and thermodynamic conditions in stellar outflows1,2,3,4,5. Novae are stellar explosions that take place in the hydrogen-rich envelope accreted onto the surface of a white dwarf in a close binary system6. The energy released by a suite of nuclear processes operating in the envelope powers a thermonuclear runaway, resulting in the ejection of processed material into the interstellar medium. Spectral fitting of features observed in the infrared spectra of dust-forming novae provided evidence of the co-condensation of both carbonaceous and silicate dust in stellar outflows within 50 to 100 days after explosion7,8,9. Although novae appear as prolific producers of both carbon- and oxygen-rich dust, very few presolar grains that can be attributed to novae have been found in meteorites thus far10,11,12,13,14,15,16. Here, we report the identification of an oxygen-rich inclusion, composed of both silicate and oxide nanoparticles, inside a graphite spherule that originated in the ejecta of a low-mass carbon- and oxygen-rich (CO) nova. This observation establishes laboratory evidence of the co-condensation of oxygen- and carbon-rich dust in nova outbursts and is consistent with large-scale transport and mixing of materials between chemically distinct clumps in the nova ejecta.
dc.language.isoeng
dc.publisherSpringer Nature
dc.rightsAttribution-NonCommercial-NoDerivs 3.0 Spain
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/
dc.subjectÀrees temàtiques de la UPC::Física::Astronomia i astrofísica
dc.subject.lcshStars
dc.titleLaboratory evidence for co-condensed oxygen- and carbon-rich meteoritic stardust from nova outbursts
dc.typeArticle
dc.subject.lemacEstels
dc.contributor.groupUniversitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica
dc.identifier.doi10.1038/s41550-019-0757-4
dc.relation.publisherversionhttps://www.nature.com/articles/s41550-019-0757-4
dc.rights.accessOpen Access
dc.description.versionPreprint
upcommons.citation.authorHaenecour, P.; Howe, J.Y.; Zega, T.J.; Amari, S.; Lodders, K.; Jose, J.; Kaji, K.; Sunaoshi, T.; Atsushi, M.
upcommons.citation.publishedtrue
upcommons.citation.publicationNameNature Astronomy


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