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Article: Independent emission and absorption abundances for planetary nebulae

TitleIndependent emission and absorption abundances for planetary nebulae
Authors
KeywordsISM: abundances
Planetary nebulae: general
Planetary nebulae: individual (He 2-138, NGC 246, NGC 6543, Tc 1)
Ultraviolet: ISM
Issue Date2008
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2008, v. 677 n. 2, p. 1100-1119 How to Cite?
AbstractEmission-line abundances have been uncertain for more than a decade due to unexplained discrepancies in the relative intensities of the forbidden lines and weak permitted recombination lines in PNe and H II regions. The observed intensities of forbidden and recombination lines originating from the same parent ion differ from their theoretical values by factors of more than an order of magnitude in some of these nebulae. In this study we observe UV resonance line absorption in the central stars of PNe produced by the nebular gas and from the same ions that emit optical forbidden lines. We then compare the derived absorption column densities with the emission measures determined from ground-based observations of the nebular forbidden lines. We find for our sample of PNe that the collisionally excited forbidden lines yield column densities that are in basic agreement with the column densities derived for the same ions from the UV absorption lines. A similar comparison involving recombination line column densities produces poorer agreement, although near the limits of the formal uncertainties of the analyses. An additional sample of objects with larger abundance discrepancy factors will need to be studied before a stronger statement can be made that recombination line abundances are not correct. © 2008. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/138793
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorWilliams, Ren_HK
dc.contributor.authorJenkins, EBen_HK
dc.contributor.authorBaldwin, JAen_HK
dc.contributor.authorZhang, Yen_HK
dc.contributor.authorSharpee, Ben_HK
dc.contributor.authorPellegrini, Een_HK
dc.contributor.authorPhillips, Men_HK
dc.date.accessioned2011-09-19T01:40:17Z-
dc.date.available2011-09-19T01:40:17Z-
dc.date.issued2008en_HK
dc.identifier.citationAstrophysical Journal Letters, 2008, v. 677 n. 2, p. 1100-1119en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/138793-
dc.description.abstractEmission-line abundances have been uncertain for more than a decade due to unexplained discrepancies in the relative intensities of the forbidden lines and weak permitted recombination lines in PNe and H II regions. The observed intensities of forbidden and recombination lines originating from the same parent ion differ from their theoretical values by factors of more than an order of magnitude in some of these nebulae. In this study we observe UV resonance line absorption in the central stars of PNe produced by the nebular gas and from the same ions that emit optical forbidden lines. We then compare the derived absorption column densities with the emission measures determined from ground-based observations of the nebular forbidden lines. We find for our sample of PNe that the collisionally excited forbidden lines yield column densities that are in basic agreement with the column densities derived for the same ions from the UV absorption lines. A similar comparison involving recombination line column densities produces poorer agreement, although near the limits of the formal uncertainties of the analyses. An additional sample of objects with larger abundance discrepancy factors will need to be studied before a stronger statement can be made that recombination line abundances are not correct. © 2008. The American Astronomical Society. All rights reserved.en_HK
dc.languageeng-
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectISM: abundancesen_HK
dc.subjectPlanetary nebulae: generalen_HK
dc.subjectPlanetary nebulae: individual (He 2-138, NGC 246, NGC 6543, Tc 1)en_HK
dc.subjectUltraviolet: ISMen_HK
dc.titleIndependent emission and absorption abundances for planetary nebulaeen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=677&issue=2&spage=1100&epage=1119&date=2008&atitle=Independent+emission+and+absorption+abundances+for+planetary+nebulae-
dc.identifier.emailZhang, Y: zhangy96@hku.hken_HK
dc.identifier.authorityZhang, Y=rp00841en_HK
dc.description.naturepublished_or_final_versionen_US
dc.identifier.doi10.1086/529065en_HK
dc.identifier.scopuseid_2-s2.0-42649102669en_HK
dc.identifier.hkuros142737-
dc.identifier.volume677en_HK
dc.identifier.issue2en_HK
dc.identifier.spage1100en_HK
dc.identifier.epage1119en_HK
dc.identifier.isiWOS:000254898000024-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridWilliams, R=7409604935en_HK
dc.identifier.scopusauthoridJenkins, EB=7202285481en_HK
dc.identifier.scopusauthoridBaldwin, JA=35184774500en_HK
dc.identifier.scopusauthoridZhang, Y=23768446500en_HK
dc.identifier.scopusauthoridSharpee, B=6602273650en_HK
dc.identifier.scopusauthoridPellegrini, E=8404989800en_HK
dc.identifier.scopusauthoridPhillips, M=7402770160en_HK

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