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Article: 2-45 micron infrared spectroscopy of carbon-rich proto-planetary nebulae

Title2-45 micron infrared spectroscopy of carbon-rich proto-planetary nebulae
Authors
KeywordsCircumstellar Matter
Infrared: Ism: Lines And Bands
Infrared: Stars
Planetary Nebulae: General
Radiative Transfer
Stars: Agb And Post-Agb
Issue Date2000
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
The Astrophysical Journal, 2000, v. 535 n. 1 pt. 1, p. 275-292 How to Cite?
AbstractInfrared Space Observatory (ISO) 2-45 μm observations of seven proto-planetary nebulae (PPNs) and two other carbon-rich objects are presented. The unidentified emission features at 21 and 30 μm are detected in six sources, including four new detections of the 30 μm feature. This previously unresolved 30 μm feature is now resolved and found to consist of a broad feature peaking at 27.2 μm (the "30 μm" feature) and a narrower feature at 25.5 μm (the "26 μm" feature). This new 26 μm feature is detected in eight sources and is particularly strong in IRAS Z02229 + 6208 and 16594-4656. The unidentified infrared (UIR) emission features at 3.3, 6.2, 7.7, and 11.3 μm, which are commonly observed in planetary nebulae and H II regions, are also seen in these PPNs. However, their strengths relative to the continuum plateaus at 8 and 12 μm are weaker than in planetary nebulae. The 6.9 μm feature, seen almost exclusively in PPNs, is strong. New millimeter CO and HCN observations were made; they support the carbon-rich nature of the objects and yield the expansion velocities of the gaseous envelopes. The spectral energy distributions of these PPNs were fitted with a radiative-transfer model, taking into account the emission features at 21, 26, and 30 μm. A significant fraction of the total energy output is emitted in these features: as high as 20% in the 30 μm feature and 8% in the 21 μm feature. The fact that so much energy is carried in these features suggests that the material responsible for these features must be made of abundant elements and most likely involves carbon. SiS 2 appears to be ruled out as the emitter of the 21 μm feature due to the absence of a predicted companion feature.
Persistent Identifierhttp://hdl.handle.net/10722/179656
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
References

 

DC FieldValueLanguage
dc.contributor.authorHrivnak, BJen_US
dc.contributor.authorVolk, Ken_US
dc.contributor.authorKwok, Sen_US
dc.date.accessioned2012-12-19T10:02:17Z-
dc.date.available2012-12-19T10:02:17Z-
dc.date.issued2000en_US
dc.identifier.citationThe Astrophysical Journal, 2000, v. 535 n. 1 pt. 1, p. 275-292en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/179656-
dc.description.abstractInfrared Space Observatory (ISO) 2-45 μm observations of seven proto-planetary nebulae (PPNs) and two other carbon-rich objects are presented. The unidentified emission features at 21 and 30 μm are detected in six sources, including four new detections of the 30 μm feature. This previously unresolved 30 μm feature is now resolved and found to consist of a broad feature peaking at 27.2 μm (the "30 μm" feature) and a narrower feature at 25.5 μm (the "26 μm" feature). This new 26 μm feature is detected in eight sources and is particularly strong in IRAS Z02229 + 6208 and 16594-4656. The unidentified infrared (UIR) emission features at 3.3, 6.2, 7.7, and 11.3 μm, which are commonly observed in planetary nebulae and H II regions, are also seen in these PPNs. However, their strengths relative to the continuum plateaus at 8 and 12 μm are weaker than in planetary nebulae. The 6.9 μm feature, seen almost exclusively in PPNs, is strong. New millimeter CO and HCN observations were made; they support the carbon-rich nature of the objects and yield the expansion velocities of the gaseous envelopes. The spectral energy distributions of these PPNs were fitted with a radiative-transfer model, taking into account the emission features at 21, 26, and 30 μm. A significant fraction of the total energy output is emitted in these features: as high as 20% in the 30 μm feature and 8% in the 21 μm feature. The fact that so much energy is carried in these features suggests that the material responsible for these features must be made of abundant elements and most likely involves carbon. SiS 2 appears to be ruled out as the emitter of the 21 μm feature due to the absence of a predicted companion feature.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637Xen_US
dc.relation.ispartofThe Astrophysical Journalen_US
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectCircumstellar Matteren_US
dc.subjectInfrared: Ism: Lines And Bandsen_US
dc.subjectInfrared: Starsen_US
dc.subjectPlanetary Nebulae: Generalen_US
dc.subjectRadiative Transferen_US
dc.subjectStars: Agb And Post-Agben_US
dc.title2-45 micron infrared spectroscopy of carbon-rich proto-planetary nebulaeen_US
dc.typeArticleen_US
dc.identifier.emailKwok, S: deannote@hku.hken_US
dc.identifier.authorityKwok, S=rp00716en_US
dc.description.naturepublished_or_final_versionen_US
dc.identifier.doi10.1086/308823-
dc.identifier.scopuseid_2-s2.0-0034690376en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0034690376&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume535en_US
dc.identifier.issue1 pt. 1en_US
dc.identifier.spage275en_US
dc.identifier.epage292en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridHrivnak, BJ=35613962100en_US
dc.identifier.scopusauthoridVolk, K=7006571965en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US

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