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Article: Physical and Chemical Properties of Planetary Nebulae with WR-type Nuclei

TitlePhysical and Chemical Properties of Planetary Nebulae with WR-type Nuclei
Authors
KeywordsAstrophysics - Solar and Stellar Astrophysics
Astrophysics - Astrophysics of Galaxies
Issue Date2014
Citation
ArXiv e-prints, 2014, v. 1411, p. 2191-2191 How to Cite?
AbstractWe have carried out optical spectroscopic measurements of emission lines for a sample of Galactic planetary nebulae with Wolf-Rayet (WR) stars and weak emission-line stars (wels). The plasma diagnostics and elemental abundance analysis have been done using both collisionally excited lines (CELs) and optical recombination lines (ORLs). It is found that the abundance discrepancy factors (ADF=ORL/CEL) are closely correlated with the dichotomy between temperatures derived from forbidden lines and those from He I recombination lines, implying the existence of H-deficient materials embedded in the nebula. The H$\beta$ surface brightness correlations suggest that they might be also related to the nebular evolution.
Persistent Identifierhttp://hdl.handle.net/10722/211191

 

DC FieldValueLanguage
dc.contributor.authorDanehkar, A-
dc.contributor.authorWesson, R-
dc.contributor.authorKarakas, A-
dc.contributor.authorParker, QA-
dc.date.accessioned2015-07-08T03:22:50Z-
dc.date.available2015-07-08T03:22:50Z-
dc.date.issued2014-
dc.identifier.citationArXiv e-prints, 2014, v. 1411, p. 2191-2191-
dc.identifier.urihttp://hdl.handle.net/10722/211191-
dc.description.abstractWe have carried out optical spectroscopic measurements of emission lines for a sample of Galactic planetary nebulae with Wolf-Rayet (WR) stars and weak emission-line stars (wels). The plasma diagnostics and elemental abundance analysis have been done using both collisionally excited lines (CELs) and optical recombination lines (ORLs). It is found that the abundance discrepancy factors (ADF=ORL/CEL) are closely correlated with the dichotomy between temperatures derived from forbidden lines and those from He I recombination lines, implying the existence of H-deficient materials embedded in the nebula. The H$\beta$ surface brightness correlations suggest that they might be also related to the nebular evolution.-
dc.languageeng-
dc.relation.ispartofArXiv e-prints-
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectAstrophysics - Solar and Stellar Astrophysics-
dc.subjectAstrophysics - Astrophysics of Galaxies-
dc.titlePhysical and Chemical Properties of Planetary Nebulae with WR-type Nuclei-
dc.typeArticle-
dc.identifier.emailParker, QA: quentinp@hku.hk-
dc.identifier.authorityParker, QA=rp02017-
dc.description.naturepostprint-
dc.identifier.volume1411-
dc.identifier.spage2191-
dc.identifier.epage2191-

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