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Conference Paper: Aromatic, aliphatic, and the unidentified 21 micron emission features in proto-planetary nebulae

TitleAromatic, aliphatic, and the unidentified 21 micron emission features in proto-planetary nebulae
Authors
KeywordsAstrochemistry
Circumstellar matter
Infrared: ISM
ISM: lines and bands
Planetary nebulae: general
Stars: AGB and post-AGB
Issue Date2008
PublisherCambridge University Press. The Journal's web site is located at http://journals.cambridge.org/action/displayJournal?jid=IAU
Citation
The International Astronomical Union (IAU) Symposium S251: Organic Matter in Space, Hong Kong, 18-22 February 2008. How to Cite?
AbstractAromatic features at 3.3, 6.2, 7.7, 8.6, 11.3 m are observed in proto-planetary nebulae (PPNe) as well as in PNe and H ii regions. Aliphatic features at 3.4 and 6.9 m are also observed; however, these features are often stronger in PPNe than in PNe. These observations suggest an evolution in the features from simple molecules (C2H2) in AGB stars to aliphatics in PPNe to aromatics in PNe. In the same carbon-rich PPNe, a strong, broad, unidentified 21 m emission feature has been found. We will present recent observations of the aromatic, aliphatic, and 21 m emission features, along with C2H2 (13.7 m) and a new feature at 15.8 m, and discuss correlations among them and other properties of these PPNe. © 2008 International Astronomical Union.
DescriptionProceedings of the International Astronomical Union, 2008, v. 4 n. S251, p. 213-214
Persistent Identifierhttp://hdl.handle.net/10722/128486
ISSN
2015 SCImago Journal Rankings: 0.105
References

 

DC FieldValueLanguage
dc.contributor.authorHrivnak, BJen_HK
dc.contributor.authorVolk, Ken_HK
dc.contributor.authorGeballe, TRen_HK
dc.contributor.authorKwok, Sen_HK
dc.date.accessioned2010-10-31T14:30:52Z-
dc.date.available2010-10-31T14:30:52Z-
dc.date.issued2008en_HK
dc.identifier.citationThe International Astronomical Union (IAU) Symposium S251: Organic Matter in Space, Hong Kong, 18-22 February 2008.en_HK
dc.identifier.issn1743-9213en_HK
dc.identifier.urihttp://hdl.handle.net/10722/128486-
dc.descriptionProceedings of the International Astronomical Union, 2008, v. 4 n. S251, p. 213-214-
dc.description.abstractAromatic features at 3.3, 6.2, 7.7, 8.6, 11.3 m are observed in proto-planetary nebulae (PPNe) as well as in PNe and H ii regions. Aliphatic features at 3.4 and 6.9 m are also observed; however, these features are often stronger in PPNe than in PNe. These observations suggest an evolution in the features from simple molecules (C2H2) in AGB stars to aliphatics in PPNe to aromatics in PNe. In the same carbon-rich PPNe, a strong, broad, unidentified 21 m emission feature has been found. We will present recent observations of the aromatic, aliphatic, and 21 m emission features, along with C2H2 (13.7 m) and a new feature at 15.8 m, and discuss correlations among them and other properties of these PPNe. © 2008 International Astronomical Union.en_HK
dc.languageengen_HK
dc.publisherCambridge University Press. The Journal's web site is located at http://journals.cambridge.org/action/displayJournal?jid=IAUen_HK
dc.relation.ispartofProceedings of the International Astronomical Unionen_HK
dc.rightsInternational Astronomical Union Proceedings. Copyright © Cambridge University Press.en_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectAstrochemistryen_HK
dc.subjectCircumstellar matteren_HK
dc.subjectInfrared: ISMen_HK
dc.subjectISM: lines and bandsen_HK
dc.subjectPlanetary nebulae: generalen_HK
dc.subjectStars: AGB and post-AGBen_HK
dc.titleAromatic, aliphatic, and the unidentified 21 micron emission features in proto-planetary nebulaeen_HK
dc.typeConference_Paperen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=1743-9213&volume=4&issue=S251&spage=213&epage=214&date=2008&atitle=Aromatic,+aliphatic,+and+the+unidentified+21+micron+emission+features+in+proto-planetary+nebulae-
dc.identifier.emailKwok, S: deannote@hku.hken_HK
dc.identifier.authorityKwok, S=rp00716en_HK
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1017/S1743921308021583en_HK
dc.identifier.scopuseid_2-s2.0-53349117820en_HK
dc.identifier.hkuros181604en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-53349117820&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume4en_HK
dc.identifier.issueS251en_HK
dc.identifier.spage213en_HK
dc.identifier.epage214en_HK
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridHrivnak, BJ=35613962100en_HK
dc.identifier.scopusauthoridVolk, K=7006571965en_HK
dc.identifier.scopusauthoridGeballe, TR=7103289480en_HK
dc.identifier.scopusauthoridKwok, S=22980498300en_HK

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