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Article: Energy distributions of symbiotic novae

TitleEnergy distributions of symbiotic novae
Authors
KeywordsInfrared: Spectra
Stars: Circumstellar Shells
Stars: Symbiotic
Ultraviolet: Spectra
Issue Date1991
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
The Astrophysical Journal, 1991, v. 368 n. 1, p. 252-260 How to Cite?
AbstractThe IRAS low-resolution spectra of three recent symbiotic novae (HM Sge. V1016 Cyg, and RR Tel) are fitted with a dust continuum radiative transfer model. We find that the dust shells are detached from the photosphere and that the sizes of the inner radii are correlated with times since outburst. An analysis of the IUE spectra of HM Sge at different epochs suggests that the strength of the 2200 Å feature is decreasing with time and the grains responsible for the feature are probably formed in the white dwarf ejecta. A complete accounting of the entire energy budget from radio to X-ray shows that most of the energy is emitted by the cool component in the infrared, and a significant fraction of the flux of the hot component is escaping in the far-ultraviolet. The density-bounded nature of the circumstellar gas nebulae could be the result of a bipolar geometry of the nebulae. Unlike classical novae, the optical outburst of symbiotic novae is due to the ionization of the preexisting envelope of the cool component and is not the result of a sudden ejection by the hot component.
Persistent Identifierhttp://hdl.handle.net/10722/179631
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorBryan, GLen_US
dc.contributor.authorKwok, Sen_US
dc.date.accessioned2012-12-19T10:02:10Z-
dc.date.available2012-12-19T10:02:10Z-
dc.date.issued1991en_US
dc.identifier.citationThe Astrophysical Journal, 1991, v. 368 n. 1, p. 252-260en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/179631-
dc.description.abstractThe IRAS low-resolution spectra of three recent symbiotic novae (HM Sge. V1016 Cyg, and RR Tel) are fitted with a dust continuum radiative transfer model. We find that the dust shells are detached from the photosphere and that the sizes of the inner radii are correlated with times since outburst. An analysis of the IUE spectra of HM Sge at different epochs suggests that the strength of the 2200 Å feature is decreasing with time and the grains responsible for the feature are probably formed in the white dwarf ejecta. A complete accounting of the entire energy budget from radio to X-ray shows that most of the energy is emitted by the cool component in the infrared, and a significant fraction of the flux of the hot component is escaping in the far-ultraviolet. The density-bounded nature of the circumstellar gas nebulae could be the result of a bipolar geometry of the nebulae. Unlike classical novae, the optical outburst of symbiotic novae is due to the ionization of the preexisting envelope of the cool component and is not the result of a sudden ejection by the hot component.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.subjectInfrared: Spectraen_US
dc.subjectStars: Circumstellar Shellsen_US
dc.subjectStars: Symbioticen_US
dc.subjectUltraviolet: Spectraen_US
dc.titleEnergy distributions of symbiotic novaeen_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.doi10.1086/169688-
dc.identifier.scopuseid_2-s2.0-0000228334en_US
dc.identifier.volume368en_US
dc.identifier.issue1en_US
dc.identifier.spage252en_US
dc.identifier.epage260en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridBryan, GL=7102268958en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US

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