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Article: Observations and three-dimensional ionization structure of the planetary nebula SuWt 2

TitleObservations and three-dimensional ionization structure of the planetary nebula SuWt 2
Authors
KeywordsISM
Abundances-planetary nebulae
Individual
PN SuWt 2
Issue Date2013
Citation
Monthly Notices of the Royal Astronomical Society, 2013, v. 434, n. 2, p. 1513-1530 How to Cite?
AbstractThe planetary nebula SuWt 2 (PN G311.0+02.4) is an unusual object with a prominent, inclined central emission ellipse and faint bipolar extensions. It has two A-type stars in a proven binary system at the centre. However, the radiation from these two central stars is too soft to ionize the surrounding material leading to a so far fruitless search for the responsible ionizing source. Such a source is clearly required and has already been inferred to exist via an observed temporal variation of the centre-of-mass velocity of the A-type stars. Moreover, the ejected nebula is nitrogen rich which raises question about the mass-loss process from a likely intermediate-mass progenitor. We use optical integral-field spectroscopy to study the emission lines of the inner nebula ring. This has enabled us to perform an empirical analysis of the optical collisionally excited lines, together with a fully three-dimensional photoionization modelling. Our empirical results are used to constrain the photoionization models, which determine the evolutionary stage of the responsible ionizing source and its likely progenitor. The time-scale for the evolutionary track of a hydrogen-rich model atmosphere is inconsistent with the dynamical age obtained for the ring. This suggests that the central star has undergone a very late thermal pulse. We conclude that the ionizing star could be hydrogen deficient and compatible with what is known as a PG 1159-type star. The evolutionary tracks for the very late thermal pulse models imply a central star mass of ~0.64M⊙, which originated from an ~3M⊙ progenitor. The evolutionary time-scales suggest that the central star left the asymptotic giant branch about 25 000 yr ago, which is consistent with the nebula's age. ©2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Persistent Identifierhttp://hdl.handle.net/10722/208973
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806

 

DC FieldValueLanguage
dc.contributor.authorDanehkar, Ashkbiz-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorErcolano, Barbara-
dc.date.accessioned2015-03-23T02:02:25Z-
dc.date.available2015-03-23T02:02:25Z-
dc.date.issued2013-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2013, v. 434, n. 2, p. 1513-1530-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/208973-
dc.description.abstractThe planetary nebula SuWt 2 (PN G311.0+02.4) is an unusual object with a prominent, inclined central emission ellipse and faint bipolar extensions. It has two A-type stars in a proven binary system at the centre. However, the radiation from these two central stars is too soft to ionize the surrounding material leading to a so far fruitless search for the responsible ionizing source. Such a source is clearly required and has already been inferred to exist via an observed temporal variation of the centre-of-mass velocity of the A-type stars. Moreover, the ejected nebula is nitrogen rich which raises question about the mass-loss process from a likely intermediate-mass progenitor. We use optical integral-field spectroscopy to study the emission lines of the inner nebula ring. This has enabled us to perform an empirical analysis of the optical collisionally excited lines, together with a fully three-dimensional photoionization modelling. Our empirical results are used to constrain the photoionization models, which determine the evolutionary stage of the responsible ionizing source and its likely progenitor. The time-scale for the evolutionary track of a hydrogen-rich model atmosphere is inconsistent with the dynamical age obtained for the ring. This suggests that the central star has undergone a very late thermal pulse. We conclude that the ionizing star could be hydrogen deficient and compatible with what is known as a PG 1159-type star. The evolutionary tracks for the very late thermal pulse models imply a central star mass of ~0.64M⊙, which originated from an ~3M⊙ progenitor. The evolutionary time-scales suggest that the central star left the asymptotic giant branch about 25 000 yr ago, which is consistent with the nebula's age. ©2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectISM-
dc.subjectAbundances-planetary nebulae-
dc.subjectIndividual-
dc.subjectPN SuWt 2-
dc.titleObservations and three-dimensional ionization structure of the planetary nebula SuWt 2-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1093/mnras/stt1116-
dc.identifier.scopuseid_2-s2.0-84882993043-
dc.identifier.volume434-
dc.identifier.issue2-
dc.identifier.spage1513-
dc.identifier.epage1530-
dc.identifier.eissn1365-2966-

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