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Article: Observations and three-dimensional ionization structure of the planetary nebula SuWt 2
Title | Observations and three-dimensional ionization structure of the planetary nebula SuWt 2 |
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Authors | |
Keywords | ISM Abundances-planetary nebulae Individual PN SuWt 2 |
Issue Date | 2013 |
Citation | Monthly Notices of the Royal Astronomical Society, 2013, v. 434, n. 2, p. 1513-1530 How to Cite? |
Abstract | The 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 Identifier | http://hdl.handle.net/10722/208973 |
ISSN | 2021 Impact Factor: 5.235 2020 SCImago Journal Rankings: 2.058 |
ISI Accession Number ID |
DC Field | Value | Language |
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dc.contributor.author | Danehkar, Ashkbiz | - |
dc.contributor.author | Parker, Quentin A. | - |
dc.contributor.author | Ercolano, Barbara | - |
dc.date.accessioned | 2015-03-23T02:02:25Z | - |
dc.date.available | 2015-03-23T02:02:25Z | - |
dc.date.issued | 2013 | - |
dc.identifier.citation | Monthly Notices of the Royal Astronomical Society, 2013, v. 434, n. 2, p. 1513-1530 | - |
dc.identifier.issn | 0035-8711 | - |
dc.identifier.uri | http://hdl.handle.net/10722/208973 | - |
dc.description.abstract | The 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.language | eng | - |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | - |
dc.subject | ISM | - |
dc.subject | Abundances-planetary nebulae | - |
dc.subject | Individual | - |
dc.subject | PN SuWt 2 | - |
dc.title | Observations and three-dimensional ionization structure of the planetary nebula SuWt 2 | - |
dc.type | Article | - |
dc.description.nature | link_to_OA_fulltext | - |
dc.identifier.doi | 10.1093/mnras/stt1116 | - |
dc.identifier.scopus | eid_2-s2.0-84882993043 | - |
dc.identifier.volume | 434 | - |
dc.identifier.issue | 2 | - |
dc.identifier.spage | 1513 | - |
dc.identifier.epage | 1530 | - |
dc.identifier.eissn | 1365-2966 | - |
dc.identifier.isi | WOS:000323638200045 | - |
dc.identifier.issnl | 0035-8711 | - |