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Article: The 30 micron emission band in carbon-rich pre-planetary nebulae

TitleThe 30 micron emission band in carbon-rich pre-planetary nebulae
Authors
KeywordsCircumstellar Matter
Dust, Extinction
Infrared: Stars
Planetary Nebulae: General
Stars: Agb And Post-Agb
Stars: Carbon
Issue Date1995
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
The Astrophysical Journal, 1995, v. 454 n. 2, p. 819-825 How to Cite?
AbstractThe 16-48 μm spectra of five carbon-rich post-AGB objects (pre-planetary nebulae, PPNs) known to have an unidentified 21 μm emission feature in their IRAS LRS spectra have been obtained using the Kuiper Airborne Observatory. A broad emission band extending from 24 to ∼45 μm is present in the spectra of these objects. Peaking at ∼30 μm, the intensity of the band is variable from source to source, accounting in one case (IRAS 22272 + 5435) for ∼20% of its bolometric luminosity. However, its strength is not correlated with that of the 21 μm feature. The 30 μm band is similar to the feature previously found in other carbon-rich AGB stars and planetary nebulae. It is thus seen in a wide variety of objects, while the 21 μm band is seen only in a subset of PPNs. It was suggested for AGB stars that the 30 μm band could be carried by solid MgS particles. The observed 30 μm emission is modeled combining distributions of carbon grains and MgS grains. The required MgS abundance with respect to H nuclei is roughly estimated to be less than ∼7 × 10 -6, i.e., representing about 50% and 25% of the total abundances of S and Mg, respectively. Despite the relatively good fit with MgS, the possibility of alternative models especially with carbon-related compounds should still be addressed.
Persistent Identifierhttp://hdl.handle.net/10722/179676
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorOmont, Aen_US
dc.contributor.authorMoseley, SHen_US
dc.contributor.authorCox, Pen_US
dc.contributor.authorGlaccum, Wen_US
dc.contributor.authorCasey, Sen_US
dc.contributor.authorForveille, Ten_US
dc.contributor.authorChan, KWen_US
dc.contributor.authorSzczerba, Ren_US
dc.contributor.authorLoewenstein, RFen_US
dc.contributor.authorHarvey, PMen_US
dc.contributor.authorKwok, Sen_US
dc.date.accessioned2012-12-19T10:02:46Z-
dc.date.available2012-12-19T10:02:46Z-
dc.date.issued1995en_US
dc.identifier.citationThe Astrophysical Journal, 1995, v. 454 n. 2, p. 819-825en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/179676-
dc.description.abstractThe 16-48 μm spectra of five carbon-rich post-AGB objects (pre-planetary nebulae, PPNs) known to have an unidentified 21 μm emission feature in their IRAS LRS spectra have been obtained using the Kuiper Airborne Observatory. A broad emission band extending from 24 to ∼45 μm is present in the spectra of these objects. Peaking at ∼30 μm, the intensity of the band is variable from source to source, accounting in one case (IRAS 22272 + 5435) for ∼20% of its bolometric luminosity. However, its strength is not correlated with that of the 21 μm feature. The 30 μm band is similar to the feature previously found in other carbon-rich AGB stars and planetary nebulae. It is thus seen in a wide variety of objects, while the 21 μm band is seen only in a subset of PPNs. It was suggested for AGB stars that the 30 μm band could be carried by solid MgS particles. The observed 30 μm emission is modeled combining distributions of carbon grains and MgS grains. The required MgS abundance with respect to H nuclei is roughly estimated to be less than ∼7 × 10 -6, i.e., representing about 50% and 25% of the total abundances of S and Mg, respectively. Despite the relatively good fit with MgS, the possibility of alternative models especially with carbon-related compounds should still be addressed.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.subjectDust, Extinctionen_US
dc.subjectInfrared: Starsen_US
dc.subjectPlanetary Nebulae: Generalen_US
dc.subjectStars: Agb And Post-Agben_US
dc.subjectStars: Carbonen_US
dc.titleThe 30 micron emission band in carbon-rich pre-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.doi10.1086/176534-
dc.identifier.scopuseid_2-s2.0-11944254092en_US
dc.identifier.volume454en_US
dc.identifier.issue2en_US
dc.identifier.spage819en_US
dc.identifier.epage825en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridOmont, A=7007143431en_US
dc.identifier.scopusauthoridMoseley, SH=7006404868en_US
dc.identifier.scopusauthoridCox, P=44561017600en_US
dc.identifier.scopusauthoridGlaccum, W=6602861181en_US
dc.identifier.scopusauthoridCasey, S=26032536700en_US
dc.identifier.scopusauthoridForveille, T=7003444714en_US
dc.identifier.scopusauthoridChan, KW=12801876900en_US
dc.identifier.scopusauthoridSzczerba, R=7004424914en_US
dc.identifier.scopusauthoridLoewenstein, RF=7004001147en_US
dc.identifier.scopusauthoridHarvey, PM=7401431985en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US

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