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Article: Morphological structures of planetary nebulae

TitleMorphological structures of planetary nebulae
Authors
KeywordsAGB and post-AGB - Stars
General - Stars
Mass loss
Planetary nebulae
Issue Date2010
PublisherC S I R O, Publishing. The Journal's web site is located at http://adswww.harvard.edu/article_service.html
Citation
Publications Of The Astronomical Society Of Australia, 2010, v. 27 n. 2, p. 174-179 How to Cite?
AbstractSince various structural components of planetary nebulae (PN) manifest themselves differently, a combination of optical, infrared, submillimetre and radio techniques is needed to derive a complete picture of planetary nebulae. The effects of projection can also make derivation of the true 3-D structure difficult. Using a number of examples, we show that bipolar and multipolar nebulae are much more common than usually inferred from morphological classifications of apparent structures of planetary nebulae. We put forward a new hypothesis that the bipolar and multipolar lobes of PN are not regions of high-density ejected matter, but the result of ionization and illumination. The visible bright regions are in fact volumes of low density (cleared by high-velocity outflows), through which UV photons are being channelled. We suggest that multipolar nebulae with similar lobe sizes are not caused by simultaneous ejection of matter in several directions, but by leakage of UV photons in those directions. © Astronomical Society of Australia 2010.
Persistent Identifierhttp://hdl.handle.net/10722/128495
ISSN
2015 Impact Factor: 3.245
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorKwok, Sen_HK
dc.date.accessioned2010-10-31T14:31:37Z-
dc.date.available2010-10-31T14:31:37Z-
dc.date.issued2010en_HK
dc.identifier.citationPublications Of The Astronomical Society Of Australia, 2010, v. 27 n. 2, p. 174-179en_HK
dc.identifier.issn1323-3580en_HK
dc.identifier.urihttp://hdl.handle.net/10722/128495-
dc.description.abstractSince various structural components of planetary nebulae (PN) manifest themselves differently, a combination of optical, infrared, submillimetre and radio techniques is needed to derive a complete picture of planetary nebulae. The effects of projection can also make derivation of the true 3-D structure difficult. Using a number of examples, we show that bipolar and multipolar nebulae are much more common than usually inferred from morphological classifications of apparent structures of planetary nebulae. We put forward a new hypothesis that the bipolar and multipolar lobes of PN are not regions of high-density ejected matter, but the result of ionization and illumination. The visible bright regions are in fact volumes of low density (cleared by high-velocity outflows), through which UV photons are being channelled. We suggest that multipolar nebulae with similar lobe sizes are not caused by simultaneous ejection of matter in several directions, but by leakage of UV photons in those directions. © Astronomical Society of Australia 2010.en_HK
dc.languageengen_HK
dc.publisherC S I R O, Publishing. The Journal's web site is located at http://adswww.harvard.edu/article_service.htmlen_HK
dc.relation.ispartofPublications of the Astronomical Society of Australiaen_HK
dc.subjectAGB and post-AGB - Starsen_HK
dc.subjectGeneral - Starsen_HK
dc.subjectMass lossen_HK
dc.subjectPlanetary nebulaeen_HK
dc.titleMorphological structures of planetary nebulaeen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=1323-3580&volume=27&issue=2&spage=174&epage=179&date=2010&atitle=Morphological+structures+of+planetary+nebulae-
dc.identifier.emailKwok, S: deannote@hku.hken_HK
dc.identifier.authorityKwok, S=rp00716en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1071/AS09027en_HK
dc.identifier.scopuseid_2-s2.0-77953164725en_HK
dc.identifier.hkuros174814en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-77953164725&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume27en_HK
dc.identifier.issue2en_HK
dc.identifier.spage174en_HK
dc.identifier.epage179en_HK
dc.identifier.isiWOS:000278133900007-
dc.publisher.placeAustraliaen_HK
dc.identifier.scopusauthoridKwok, S=22980498300en_HK

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