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Conference Paper: Helium recombination lines as a probe of abundance and temperature problems

TitleHelium recombination lines as a probe of abundance and temperature problems
Authors
KeywordsPlanetary Nebulae
Issue Date2005
Citation
Revista Mexicana De Astronomia Y Astrofisica: Serie De Conferencias, 2005, v. 23, p. 15-18 How to Cite?
AbstractThe paper presents a simplified formula to determine an electron temperature, T e(He I), for planetary nebulae (PNe) using the He I λ7281/λ6678 line flux ratio. In our previous studies of T e(He I) (Zhang et al. 2005), we used the He I line emission coeffcients given by Benjamin et al. (1999). Here we examine the results of using more recent atomic data presented by Porter et al. (2005). A good agreement is shown, suggesting that the effect of uncertainties of atomic data on the resultant Te(He I) is negligible. We also present an analytical formula to derive electron temperature using the He I discontinuity at 3421 Å. Our analysis shows that T e(He I) values are significantly lower than electron temperatures deduced from the Balmer jump of H I recombination spectra, T e(H I),and that inferred from the collisionally excited [O III] nebular-to-auroral forbidden line flux ratio, T e([O III]). In addition, T e(H I) covers a wider range of values than either T e(He I) or T e([O III]). This supports the two-abundance nebular model with hydrogen-deficient material embedded in diffuse gas of a "normal" chemical composition (i.e. ̃ solar). Copyright 2005: IA, UNAM.
Persistent Identifierhttp://hdl.handle.net/10722/176182
ISSN
References

 

DC FieldValueLanguage
dc.contributor.authorZhang, Yen_US
dc.contributor.authorRubin, RHen_US
dc.contributor.authorLiu, XWen_US
dc.date.accessioned2012-11-26T09:06:40Z-
dc.date.available2012-11-26T09:06:40Z-
dc.date.issued2005en_US
dc.identifier.citationRevista Mexicana De Astronomia Y Astrofisica: Serie De Conferencias, 2005, v. 23, p. 15-18en_US
dc.identifier.issn1405-2059en_US
dc.identifier.urihttp://hdl.handle.net/10722/176182-
dc.description.abstractThe paper presents a simplified formula to determine an electron temperature, T e(He I), for planetary nebulae (PNe) using the He I λ7281/λ6678 line flux ratio. In our previous studies of T e(He I) (Zhang et al. 2005), we used the He I line emission coeffcients given by Benjamin et al. (1999). Here we examine the results of using more recent atomic data presented by Porter et al. (2005). A good agreement is shown, suggesting that the effect of uncertainties of atomic data on the resultant Te(He I) is negligible. We also present an analytical formula to derive electron temperature using the He I discontinuity at 3421 Å. Our analysis shows that T e(He I) values are significantly lower than electron temperatures deduced from the Balmer jump of H I recombination spectra, T e(H I),and that inferred from the collisionally excited [O III] nebular-to-auroral forbidden line flux ratio, T e([O III]). In addition, T e(H I) covers a wider range of values than either T e(He I) or T e([O III]). This supports the two-abundance nebular model with hydrogen-deficient material embedded in diffuse gas of a "normal" chemical composition (i.e. ̃ solar). Copyright 2005: IA, UNAM.en_US
dc.languageengen_US
dc.relation.ispartofRevista Mexicana de Astronomia y Astrofisica: Serie de Conferenciasen_US
dc.subjectPlanetary Nebulaeen_US
dc.titleHelium recombination lines as a probe of abundance and temperature problemsen_US
dc.typeConference_Paperen_US
dc.identifier.emailZhang, Y: zhangy96@hku.hken_US
dc.identifier.authorityZhang, Y=rp00841en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-33845546831en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33845546831&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume23en_US
dc.identifier.spage15en_US
dc.identifier.epage18en_US
dc.identifier.scopusauthoridZhang, Y=23768446500en_US
dc.identifier.scopusauthoridRubin, RH=14024741900en_US
dc.identifier.scopusauthoridLiu, XW=7409287288en_US

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