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Article: Chemical abundances for Hf 2-2, a planetary nebula with the strongest-known heavy-element recombination lines

TitleChemical abundances for Hf 2-2, a planetary nebula with the strongest-known heavy-element recombination lines
Authors
KeywordsIsm: Abundances
Planetary Nebulae: Individual: Hf 2-2
Issue Date2006
PublisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR
Citation
Monthly Notices Of The Royal Astronomical Society, 2006, v. 368 n. 4, p. 1959-1970 How to Cite?
AbstractWe present high-quality optical spectroscopic observations of the planetary nebula (PN) Hf 2-2. The spectrum exhibits many prominent optical recombination lines (ORLs) from heavy-element ions. Analysis of the H i and He i recombination spectrum yields an electron temperature of ∼900 K, a factor of 10 lower than given by the collisionally excited [O iii] forbidden lines. The ionic abundances of heavy elements relative to hydrogen derived from ORLs are about a factor of 70 higher than those deduced from collisionally excited lines (CELs) from the same ions, the largest abundance discrepancy factor (adf) ever measured for a PN. By comparing the observed O iiλ4089/λ4649 ORL ratio to theoretical value as a function of electron temperature, we show that the O ii ORLs arise from ionized regions with an electron temperature of only ∼630 K. The current observations thus provide the strongest evidence that the nebula contains another previously unknown component of cold, high-metallicity gas, which is too cool to excite any significant optical or ultraviolet CELs and is thus invisible via such lines. The existence of such a plasma component in PNe provides a natural solution to the long-standing dichotomy between nebular plasma diagnostics and abundance determinations using CELs on the one hand and ORLs on the other. © 2006 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/175013
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorLiu, XWen_US
dc.contributor.authorBarlow, MJen_US
dc.contributor.authorZhang, Yen_US
dc.contributor.authorBastin, RJen_US
dc.contributor.authorStorey, PJen_US
dc.date.accessioned2012-11-26T08:48:46Z-
dc.date.available2012-11-26T08:48:46Z-
dc.date.issued2006en_US
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society, 2006, v. 368 n. 4, p. 1959-1970en_US
dc.identifier.issn0035-8711en_US
dc.identifier.urihttp://hdl.handle.net/10722/175013-
dc.description.abstractWe present high-quality optical spectroscopic observations of the planetary nebula (PN) Hf 2-2. The spectrum exhibits many prominent optical recombination lines (ORLs) from heavy-element ions. Analysis of the H i and He i recombination spectrum yields an electron temperature of ∼900 K, a factor of 10 lower than given by the collisionally excited [O iii] forbidden lines. The ionic abundances of heavy elements relative to hydrogen derived from ORLs are about a factor of 70 higher than those deduced from collisionally excited lines (CELs) from the same ions, the largest abundance discrepancy factor (adf) ever measured for a PN. By comparing the observed O iiλ4089/λ4649 ORL ratio to theoretical value as a function of electron temperature, we show that the O ii ORLs arise from ionized regions with an electron temperature of only ∼630 K. The current observations thus provide the strongest evidence that the nebula contains another previously unknown component of cold, high-metallicity gas, which is too cool to excite any significant optical or ultraviolet CELs and is thus invisible via such lines. The existence of such a plasma component in PNe provides a natural solution to the long-standing dichotomy between nebular plasma diagnostics and abundance determinations using CELs on the one hand and ORLs on the other. © 2006 RAS.en_US
dc.languageengen_US
dc.publisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNRen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.subjectIsm: Abundancesen_US
dc.subjectPlanetary Nebulae: Individual: Hf 2-2en_US
dc.titleChemical abundances for Hf 2-2, a planetary nebula with the strongest-known heavy-element recombination linesen_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.doi10.1111/j.1365-2966.2006.10283.xen_US
dc.identifier.scopuseid_2-s2.0-33744536281en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33744536281&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume368en_US
dc.identifier.issue4en_US
dc.identifier.spage1959en_US
dc.identifier.epage1970en_US
dc.identifier.isiWOS:000237812700042-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridLiu, XW=7409287288en_US
dc.identifier.scopusauthoridBarlow, MJ=18041819500en_US
dc.identifier.scopusauthoridZhang, Y=23768446500en_US
dc.identifier.scopusauthoridBastin, RJ=13805498100en_US
dc.identifier.scopusauthoridStorey, PJ=7005203247en_US
dc.identifier.citeulike2794117-

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