File Download
There are no files associated with this item.
Links for fulltext
(May Require Subscription)
- Publisher Website: 10.1051/0004-6361:200809381
- Scopus: eid_2-s2.0-46649098696
- WOS: WOS:000257328600020
- Find via
Supplementary
- Citations:
- Appears in Collections:
Article: Emission line profiles as a probe of physical conditions in planetary nebulae
Title | Emission line profiles as a probe of physical conditions in planetary nebulae |
---|---|
Authors | |
Keywords | ISM: planetary nebulae: general Line: profiles |
Issue Date | 2008 |
Publisher | E 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? |
Abstract | Aims. 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 Identifier | http://hdl.handle.net/10722/59573 |
ISSN | 2023 Impact Factor: 5.4 2023 SCImago Journal Rankings: 1.896 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Zhang, Y | en_HK |
dc.date.accessioned | 2010-05-31T03:53:03Z | - |
dc.date.available | 2010-05-31T03:53:03Z | - |
dc.date.issued | 2008 | en_HK |
dc.identifier.citation | Astronomy And Astrophysics, 2008, v. 486 n. 1, p. 221-228 | en_HK |
dc.identifier.issn | 0004-6361 | en_HK |
dc.identifier.uri | http://hdl.handle.net/10722/59573 | - |
dc.description.abstract | Aims. 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.language | eng | en_HK |
dc.publisher | E D P Sciences. The Journal's web site is located at http://www.aanda.org | en_HK |
dc.relation.ispartof | Astronomy and Astrophysics | en_HK |
dc.subject | ISM: planetary nebulae: general | en_HK |
dc.subject | Line: profiles | en_HK |
dc.title | Emission line profiles as a probe of physical conditions in planetary nebulae | en_HK |
dc.type | Article | en_HK |
dc.identifier.openurl | http://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+nebulae | en_HK |
dc.identifier.email | Zhang, Y: zhangy96@hku.hk | en_HK |
dc.identifier.authority | Zhang, Y=rp00841 | en_HK |
dc.description.nature | link_to_subscribed_fulltext | - |
dc.identifier.doi | 10.1051/0004-6361:200809381 | en_HK |
dc.identifier.scopus | eid_2-s2.0-46649098696 | en_HK |
dc.identifier.hkuros | 156131 | en_HK |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-46649098696&selection=ref&src=s&origin=recordpage | en_HK |
dc.identifier.volume | 486 | en_HK |
dc.identifier.issue | 1 | en_HK |
dc.identifier.spage | 221 | en_HK |
dc.identifier.epage | 228 | en_HK |
dc.identifier.isi | WOS:000257328600020 | - |
dc.publisher.place | France | en_HK |
dc.identifier.scopusauthorid | Zhang, Y=23768446500 | en_HK |
dc.identifier.issnl | 0004-6361 | - |