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Article: Abundances of s-process elements in planetary nebulae: Br, Kr & Xe

TitleAbundances of s-process elements in planetary nebulae: Br, Kr & Xe
Authors
Zhang, YWilliams, RPellegrini, ECavagnolo, KBaldwin, JASharpee, BPhillips, MLiu, XW
KeywordsIsm: Abundances
Nucleosynthesis
Planetary Nebulae: General
Issue Date2006
PublisherCambridge University Press. The Journal's web site is located at http://journals.cambridge.org/action/displayJournal?jid=IAU
Citation
Proceedings Of The International Astronomical Union, 2006, v. 2 n. 234, p. 549-550 How to Cite?
DOI: http://dx.doi.org/10.1017/S1743921306004182
AbstractWe identify emission lines of post-iron peak elements in very high signal-to-noise spectra of a sample of planetary nebulae. Analysis of lines from ions of Kr and Xe reveals enhancements in most of the PNe, in agreement with theories of s-process in AGB stars. Surprisingly, we did not detect lines from Br even though s-process calculations indicate that it should be produced with Kr at detectable levels. © 2006 International Astronomical Union.
Persistent Identifierhttp://hdl.handle.net/10722/175046
ISSN
1743-9213
2020 SCImago Journal Rankings: 0.124
References
References in Scopus

 

DC FieldValueLanguage
dc.contributor.authorZhang, Yen_US
dc.contributor.authorWilliams, Ren_US
dc.contributor.authorPellegrini, Een_US
dc.contributor.authorCavagnolo, Ken_US
dc.contributor.authorBaldwin, JAen_US
dc.contributor.authorSharpee, Ben_US
dc.contributor.authorPhillips, Men_US
dc.contributor.authorLiu, XWen_US
dc.date.accessioned2012-11-26T08:48:56Z-
dc.date.available2012-11-26T08:48:56Z-
dc.date.issued2006en_US
dc.identifier.citationProceedings Of The International Astronomical Union, 2006, v. 2 n. 234, p. 549-550en_US
dc.identifier.issn1743-9213en_US
dc.identifier.urihttp://hdl.handle.net/10722/175046-
dc.description.abstractWe identify emission lines of post-iron peak elements in very high signal-to-noise spectra of a sample of planetary nebulae. Analysis of lines from ions of Kr and Xe reveals enhancements in most of the PNe, in agreement with theories of s-process in AGB stars. Surprisingly, we did not detect lines from Br even though s-process calculations indicate that it should be produced with Kr at detectable levels. © 2006 International Astronomical Union.en_US
dc.languageengen_US
dc.publisherCambridge University Press. The Journal's web site is located at http://journals.cambridge.org/action/displayJournal?jid=IAUen_US
dc.relation.ispartofProceedings of the International Astronomical Unionen_US
dc.subjectIsm: Abundancesen_US
dc.subjectNucleosynthesisen_US
dc.subjectPlanetary Nebulae: Generalen_US
dc.titleAbundances of s-process elements in planetary nebulae: Br, Kr & Xeen_US
dc.typeArticleen_US
dc.identifier.emailZhang, Y: zhangy96@hku.hken_US
dc.identifier.authorityZhang, Y=rp00841en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1017/S1743921306004182en_US
dc.identifier.scopuseid_2-s2.0-33845548585en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33845548585&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume2en_US
dc.identifier.issue234en_US
dc.identifier.spage549en_US
dc.identifier.epage550en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridZhang, Y=23768446500en_US
dc.identifier.scopusauthoridWilliams, R=7409604935en_US
dc.identifier.scopusauthoridPellegrini, E=8404989800en_US
dc.identifier.scopusauthoridCavagnolo, K=14059537100en_US
dc.identifier.scopusauthoridBaldwin, JA=35184774500en_US
dc.identifier.scopusauthoridSharpee, B=6602273650en_US
dc.identifier.scopusauthoridPhillips, M=7402770160en_US
dc.identifier.scopusauthoridLiu, XW=7409287288en_US
dc.identifier.issnl1743-9213-

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