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Article: Radio morphologies of planetary nebulae

TitleRadio morphologies of planetary nebulae
Authors
KeywordsPlanetary Nebulae: General
Issue Date1996
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
The Astrophysical Journal, 1996, v. 462 n. 2 pt. 1, p. 813-824 How to Cite?
AbstractWe have examined the morphologies of planetary nebulae observed in the recent very large array (VLA) surveys. The high angular resolution of the VLA has allowed the.extension of morphological classification to a much more compact population than before. The radio images of planetary nebulae are analyzed in terms of the prolate ellipsoidal shell (PES) model. Simulated radio images are produced using various asymmetry parameters in the PES model. Using these models as a guide, the radio images of planetary nebulae are classified into different morphological classes. No significant differences can be found between the statistics of morphological classes of high surface brightness/compact and low surface brightness/extended planetary nebulae, or with those classified by optical means. We conclude that the morphology of planetary nebulae is determined early in their evolution. The degree of asymmetry planetary nebulae inherited from their asymptotic giant branch progenitors is probably as important in determining the asymmetry observed in planetary nebulae as the shaping done by interacting winds during the planetary nebula phase. © 1996. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/179683
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
References

 

DC FieldValueLanguage
dc.contributor.authorAaquist, OBen_US
dc.contributor.authorKwok, Sen_US
dc.date.accessioned2012-12-19T10:02:49Z-
dc.date.available2012-12-19T10:02:49Z-
dc.date.issued1996en_US
dc.identifier.citationThe Astrophysical Journal, 1996, v. 462 n. 2 pt. 1, p. 813-824en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/179683-
dc.description.abstractWe have examined the morphologies of planetary nebulae observed in the recent very large array (VLA) surveys. The high angular resolution of the VLA has allowed the.extension of morphological classification to a much more compact population than before. The radio images of planetary nebulae are analyzed in terms of the prolate ellipsoidal shell (PES) model. Simulated radio images are produced using various asymmetry parameters in the PES model. Using these models as a guide, the radio images of planetary nebulae are classified into different morphological classes. No significant differences can be found between the statistics of morphological classes of high surface brightness/compact and low surface brightness/extended planetary nebulae, or with those classified by optical means. We conclude that the morphology of planetary nebulae is determined early in their evolution. The degree of asymmetry planetary nebulae inherited from their asymptotic giant branch progenitors is probably as important in determining the asymmetry observed in planetary nebulae as the shaping done by interacting winds during the planetary nebula phase. © 1996. The American Astronomical Society. All rights reserved.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.subjectPlanetary Nebulae: Generalen_US
dc.titleRadio morphologies of 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.doi10.1086/177196-
dc.identifier.scopuseid_2-s2.0-21344439754en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-21344439754&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume462en_US
dc.identifier.issue2 pt. 1en_US
dc.identifier.spage813en_US
dc.identifier.epage824en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridAaquist, OB=12789145800en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US

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