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Article: S-Process abundances in planetary nebulae

TitleS-Process abundances in planetary nebulae
Authors
KeywordsIsm: Abundances
Nuclear Reactions, Nucleosynthesis, Abundances
Planetary Nebulae: General
Issue Date2007
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2007, v. 659 n. 2 I, p. 1265-1290 How to Cite?
AbstractThe s-process should occur in all but the lower mass progenitor stars of planetary nebulae, and this should be reflected in the chemical composition of the gas that is expelled to create the current planetary nebula shell. Weak forbidden emission lines are expected from several s-process elements in these shells and have been searched for and in some cases detected in previous investigations. Here we extend these studies by combining very high signal-to-noise ratio echelle spectra of a sample of PNe with a critical analysis of the identification of the emission lines of Z > 30 ions. Emission lines of Br, Kr, Xe, Rb, Ba, and Pb are detected with a reasonable degree of certainty in at least some of the objects studied here, and we also tentatively identify lines from Te and I, each in one object. The strengths of these lines indicate enhancement of s-process elements in the central star progenitors, and we determine the abundances of Br, Kr, and Xe, elements for which atomic data relevant for abundance determination have recently become available. As representative elements of the "light" and "heavy " s-process peaks, Kr and Xe exhibit similar enhancements over solar values, suggesting that PN progenitors experience substantial neutron exposure. © 2007. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175065
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorSharpee, Ben_US
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.authorPhillips, Men_US
dc.contributor.authorLiu, XWen_US
dc.date.accessioned2012-11-26T08:49:04Z-
dc.date.available2012-11-26T08:49:04Z-
dc.date.issued2007en_US
dc.identifier.citationAstrophysical Journal Letters, 2007, v. 659 n. 2 I, p. 1265-1290en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175065-
dc.description.abstractThe s-process should occur in all but the lower mass progenitor stars of planetary nebulae, and this should be reflected in the chemical composition of the gas that is expelled to create the current planetary nebula shell. Weak forbidden emission lines are expected from several s-process elements in these shells and have been searched for and in some cases detected in previous investigations. Here we extend these studies by combining very high signal-to-noise ratio echelle spectra of a sample of PNe with a critical analysis of the identification of the emission lines of Z > 30 ions. Emission lines of Br, Kr, Xe, Rb, Ba, and Pb are detected with a reasonable degree of certainty in at least some of the objects studied here, and we also tentatively identify lines from Te and I, each in one object. The strengths of these lines indicate enhancement of s-process elements in the central star progenitors, and we determine the abundances of Br, Kr, and Xe, elements for which atomic data relevant for abundance determination have recently become available. As representative elements of the "light" and "heavy " s-process peaks, Kr and Xe exhibit similar enhancements over solar values, suggesting that PN progenitors experience substantial neutron exposure. © 2007. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectIsm: Abundancesen_US
dc.subjectNuclear Reactions, Nucleosynthesis, Abundancesen_US
dc.subjectPlanetary Nebulae: Generalen_US
dc.titleS-Process abundances in planetary nebulaeen_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.doi10.1086/511665en_US
dc.identifier.scopuseid_2-s2.0-34248357841en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-34248357841&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume659en_US
dc.identifier.issue2 Ien_US
dc.identifier.spage1265en_US
dc.identifier.epage1290en_US
dc.identifier.isiWOS:000245774700031-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridSharpee, B=6602273650en_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.scopusauthoridPhillips, M=7402770160en_US
dc.identifier.scopusauthoridLiu, XW=7409287288en_US

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