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Conference Paper: Revealing the Location of the Mixing Layer in a Hot Bubble

TitleRevealing the Location of the Mixing Layer in a Hot Bubble
Authors
Guerrero, MAFang, XChu, YHToala, JAGruendl, RA
Keywords(ISM:) planetary nebulae: individual (NGC 6543)
outflows
stars: winds
ultraviolet: ISM
Issue Date2016
PublisherCambridge University Press. The Journal's web site is located at http://journals.cambridge.org/action/displayJournal?jid=IAU
Citation
International Astronomical Union Symposium 323 (IAUS323): Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution, Beijing, China, 10-14 October 2016. In Proceedings of the International Astronomical Union, 2016, v. 12 n. S323, p. 114-118 How to Cite?
DOI: http://dx.doi.org/10.1017/S1743921317002320
AbstractThe fast stellar winds can blow bubbles in the circumstellar material ejected from previous phases of stellar evolution. These are found at different scales, from planetary nebulae (PNe) around stars evolving to the white dwarf stage, to Wolf-Rayet (WR) bubbles and up to large-scale bubbles around massive star clusters. In all cases, the fast stellar wind is shock-heated and a hot bubble is produced. Processes of mass evaporation and mixing of nebular material and heat conduction occurring at the mixing layer between the hot bubble and the optical nebula are key to determine the thermal structure of these bubbles and their evolution. In this contribution we review our current understanding of the X-ray observations of hot bubbles in PNe and present the first spatially-resolved study of a mixing layer in a PN.
Persistent Identifierhttp://hdl.handle.net/10722/248884
ISSN
1743-9213
2020 SCImago Journal Rankings: 0.124
ISI Accession Number ID
WOS:000456283100019

 

DC FieldValueLanguage
dc.contributor.authorGuerrero, MA-
dc.contributor.authorFang, X-
dc.contributor.authorChu, YH-
dc.contributor.authorToala, JA-
dc.contributor.authorGruendl, RA-
dc.date.accessioned2017-10-18T08:50:01Z-
dc.date.available2017-10-18T08:50:01Z-
dc.date.issued2016-
dc.identifier.citationInternational Astronomical Union Symposium 323 (IAUS323): Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution, Beijing, China, 10-14 October 2016. In Proceedings of the International Astronomical Union, 2016, v. 12 n. S323, p. 114-118-
dc.identifier.issn1743-9213-
dc.identifier.urihttp://hdl.handle.net/10722/248884-
dc.description.abstractThe fast stellar winds can blow bubbles in the circumstellar material ejected from previous phases of stellar evolution. These are found at different scales, from planetary nebulae (PNe) around stars evolving to the white dwarf stage, to Wolf-Rayet (WR) bubbles and up to large-scale bubbles around massive star clusters. In all cases, the fast stellar wind is shock-heated and a hot bubble is produced. Processes of mass evaporation and mixing of nebular material and heat conduction occurring at the mixing layer between the hot bubble and the optical nebula are key to determine the thermal structure of these bubbles and their evolution. In this contribution we review our current understanding of the X-ray observations of hot bubbles in PNe and present the first spatially-resolved study of a mixing layer in a PN.-
dc.languageeng-
dc.publisherCambridge University Press. The Journal's web site is located at http://journals.cambridge.org/action/displayJournal?jid=IAU-
dc.relation.ispartofProceedings of the International Astronomical Union-
dc.rightsProceedings of the International Astronomical Union. Copyright © Cambridge University Press.-
dc.rightsThis article has been published in a revised form in [Journal] [http://doi.org/XXX]. This version is free to view and download for private research and study only. Not for re-distribution, re-sale or use in derivative works. © copyright holder.-
dc.subject(ISM:) planetary nebulae: individual (NGC 6543)-
dc.subjectoutflows-
dc.subjectstars: winds-
dc.subjectultraviolet: ISM-
dc.titleRevealing the Location of the Mixing Layer in a Hot Bubble-
dc.typeConference_Paper-
dc.identifier.emailFang, X: fangx@hku.hk-
dc.identifier.doi10.1017/S1743921317002320-
dc.identifier.scopuseid_2-s2.0-85047224678-
dc.identifier.hkuros282341-
dc.identifier.volume12-
dc.identifier.issueS323-
dc.identifier.spage114-
dc.identifier.epage118-
dc.identifier.isiWOS:000456283100019-
dc.publisher.placeUnited Kingdom-
dc.identifier.issnl1743-9213-

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