File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Emission line profiles as a probe of physical conditions in planetary nebulae

TitleEmission line profiles as a probe of physical conditions in planetary nebulae
Authors
KeywordsISM: planetary nebulae: general
Line: profiles
Issue Date2008
PublisherE D P Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy And Astrophysics, 2008, v. 486 n. 1, p. 221-228 How to Cite?
AbstractAims. We present an analysis of physical conditions in planetary nebulae (PNe) in terms of collisionally-excited line (CEL) and optical-recombination line (ORL) profiles. We aim to investigate whether line profiles could be used to study the long-standing CEL/ORL abundance-discrepancy problem in nebular astrophysics. Methods. Using 1D photoionization models and their assumed velocity fields, we simulate the line profiles of various ionic species. We attempt to use our model to account for the observed CEL and ORL profiles. As a case study we present a detailed study of line profiles of the low-excitation planetary nebula (PN) IC 418.Results. Our results show that the profiles of classical temperature and density diagnostic lines, such as [O iii] 4363, 5007, [S ii] 6716, 6731, and [Ar iv] 4711, 4740, provide a powerful tool to study nebular temperature and density variations. The method enables the CEL/ORL abundance-discrepancy problem to be studied more rigorously than before. A pure photoionization model of a chemically-homogeneous nebula seems to explain the observed disagreements in the profiles for the [O iii] 4363 and the 5007 lines, but cannot account for the differences between the [O iii] CELs and the O ii ORLs. We also investigate the temperature and density variations in the velocity space of a sample of PNe, which are found to be insignificant. © 2008 ESO.
Persistent Identifierhttp://hdl.handle.net/10722/59573
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorZhang, Yen_HK
dc.date.accessioned2010-05-31T03:53:03Z-
dc.date.available2010-05-31T03:53:03Z-
dc.date.issued2008en_HK
dc.identifier.citationAstronomy And Astrophysics, 2008, v. 486 n. 1, p. 221-228en_HK
dc.identifier.issn0004-6361en_HK
dc.identifier.urihttp://hdl.handle.net/10722/59573-
dc.description.abstractAims. We present an analysis of physical conditions in planetary nebulae (PNe) in terms of collisionally-excited line (CEL) and optical-recombination line (ORL) profiles. We aim to investigate whether line profiles could be used to study the long-standing CEL/ORL abundance-discrepancy problem in nebular astrophysics. Methods. Using 1D photoionization models and their assumed velocity fields, we simulate the line profiles of various ionic species. We attempt to use our model to account for the observed CEL and ORL profiles. As a case study we present a detailed study of line profiles of the low-excitation planetary nebula (PN) IC 418.Results. Our results show that the profiles of classical temperature and density diagnostic lines, such as [O iii] 4363, 5007, [S ii] 6716, 6731, and [Ar iv] 4711, 4740, provide a powerful tool to study nebular temperature and density variations. The method enables the CEL/ORL abundance-discrepancy problem to be studied more rigorously than before. A pure photoionization model of a chemically-homogeneous nebula seems to explain the observed disagreements in the profiles for the [O iii] 4363 and the 5007 lines, but cannot account for the differences between the [O iii] CELs and the O ii ORLs. We also investigate the temperature and density variations in the velocity space of a sample of PNe, which are found to be insignificant. © 2008 ESO.en_HK
dc.languageengen_HK
dc.publisherE D P Sciences. The Journal's web site is located at http://www.aanda.orgen_HK
dc.relation.ispartofAstronomy and Astrophysicsen_HK
dc.subjectISM: planetary nebulae: generalen_HK
dc.subjectLine: profilesen_HK
dc.titleEmission line profiles as a probe of physical conditions in planetary nebulaeen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-6361&volume=486&spage=221&epage=228&date=2008&atitle=Emission+line+profiles+as+a+probe+of+physical+conditions+in+planetary+nebulaeen_HK
dc.identifier.emailZhang, Y: zhangy96@hku.hken_HK
dc.identifier.authorityZhang, Y=rp00841en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1051/0004-6361:200809381en_HK
dc.identifier.scopuseid_2-s2.0-46649098696en_HK
dc.identifier.hkuros156131en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-46649098696&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume486en_HK
dc.identifier.issue1en_HK
dc.identifier.spage221en_HK
dc.identifier.epage228en_HK
dc.identifier.isiWOS:000257328600020-
dc.publisher.placeFranceen_HK
dc.identifier.scopusauthoridZhang, Y=23768446500en_HK

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats