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dc.contributor.authorCasassus, S.
dc.contributor.authorRoche, P.F.
dc.contributor.authorAitken, D.
dc.contributor.authorSmith, C.H.
dc.date.accessioned2007-10-16T13:41:37Z
dc.date.available2007-10-16T13:41:37Z
dc.date.issued2001
dc.identifier.citationCasassus , S , Roche , P F , Aitken , D & Smith , C H 2001 , ' 8-13 micron dust emission features in Galactic bulge planetary nebulae ' , Monthly Notices of the Royal Astronomical Society , vol. 327 , no. 3 , pp. 744-750 . https://doi.org/10.1046/j.1365-8711.2001.04750.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 163410
dc.identifier.otherPURE UUID: 096c6663-1328-48e9-a3f1-aae00ff09fad
dc.identifier.otherdspace: 2299/923
dc.identifier.otherScopus: 0042914407
dc.identifier.urihttp://hdl.handle.net/2299/923
dc.descriptionThe definitive version is available at www.blackwell-synergy.com '. Copyright Blackwell Publishing. DOI : 10.1046/j.1365-8711.2001.04750.x
dc.description.abstractA sample of 25 IR-bright planetary nebulae (PNe) towards the Galactic bulge is analysed through 8–13μm spectroscopy. The classification of the warm-dust emission features provides a measure of the C/O chemical balance, and represents the first C/O estimates for bulge PNe. Out of 13 PNe with identified dust types, 4 PNe have emission features associated with C-based grains, while the remaining 9 have O-rich dust signatures. The low fraction of C-rich PNe, <∼ 30%, contrasts with that for local PNe, around 80%, although it follows the trend for a decreasing frequency of C-rich PNe with galactocentric radius (paper I). We investigate whether the PNe discussed here are linked to the bulge stellar population (similar to type IV, or halo, PNe) or the inner Galactic disk (a young and super-metal-rich population). Although 60% of the PNe with warm dust are convincing bulge members, none of the C-rich PNe satisfy our criteria, and they are probably linked to the inner Galactic disk. In the framework of single star evolution, the available information on bulge PNe points towards a progenitor population similar in age to that of local PNe (type I PNe are found in similar proportions), but super-metal-rich (to account for the scarcity of C-rich objects). Yet the metallicities of bulge PNe, as inferred from [O/H], fail to reach the required values - except for the C-rich objects. It is likely that the sample discussed here is derived from a mixed disk/bulge progenitor population and dominated by type IV PNe, as suggested by Peimbert (1992). The much higher fraction of O-rich PNe in this sample than in the solar neighbourhood should result in a proportionally greater injection of silicate grains into the inner Galactic medium.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.title8-13 micron dust emission features in Galactic bulge planetary nebulaeen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2001
rioxxterms.versionofrecordhttps://doi.org/10.1046/j.1365-8711.2001.04750.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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