HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula

Planetary nebulae (PNe) are expected to have a ∼10 K interface layer between the ≥10 K inner hot bubble and the ∼10 K optical nebular shell. The PN structure and evolution, and the X-ray emission, depend critically on the efficiency of the mixing of material at this interface layer. However, neither...

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Autores: Fang, Xuan, Guerrero, Martín A., Toalá, Jesús A., Chu, You-Hua, Gruendl, Robert A.
Tipo de recurso: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2016
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/381036
Acceso en línea:http://hdl.handle.net/10261/381036
Access Level:acceso abierto
Palabra clave:Planetary nebulae: general
Planetary nebulae: individual (NGC 6543)
Stars: winds, outflows
X-rays: ISM
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spelling HST STIS Observations of the Mixing Layer in the Cat’s Eye NebulaFang, XuanGuerrero, Martín A.Toalá, Jesús A.Chu, You-HuaGruendl, Robert A.Planetary nebulae: generalPlanetary nebulae: individual (NGC 6543)Stars: winds, outflowsX-rays: ISMPlanetary nebulae (PNe) are expected to have a ∼10 K interface layer between the ≥10 K inner hot bubble and the ∼10 K optical nebular shell. The PN structure and evolution, and the X-ray emission, depend critically on the efficiency of the mixing of material at this interface layer. However, neither its location nor its spatial extent have ever been determined. Using high-spatial resolution HST STIS spectroscopic observations of the N v λλ 1239,1243 lines in the Cat's Eye Nebula (NGC 6543), we have detected this interface layer and determined its location, extent, and physical properties for the first time in a PN. We confirm that this interface layer, as revealed by the spatial distribution of the N v λ1239 line emission, is located between the hot bubble and the optical nebular shell. We estimate a thickness of 1.5 × 10 cm and an electron density of ∼200 cm for the mixing layer. With a thermal pressure of ∼2 × 10 yncm, the mixing layer is in pressure equilibrium with the hot bubble and ionized nebular rim of NGC 6543. © 2016. The American Astronomical Society. All rights reserved.Support for the Hubble Space Telescope Cycle 20 General Observer Program 12509 was provided by NASA through grant HST-GO-12509.01-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. X.F., M.A.G., and J.A.T. are partially funded by grant AYA 2011-29754-C03-02 of the Spanish MEC (Ministerio de Economía y Competitividad), cofunded with FEDER funds. We thank Yong Zhang at the University of Hong Kong for discussions. This paper utilizes images from the Chandra X-ray Center (http://chandra.harvard.edu/), which was operated for NASA by the Smithsonian Astrophysical Observatory and developed with funding from NASA under contract NAS8-03060. This research has made use of NASA's Astrophysics Data System (http://adsabs.harvard.edu) and the Mikulski Archive for Space Telescope (MAST, https://archive.stsci.edu/).Peer reviewedIOP PublishingNASAEuropean CommissionMinisterio de Economía y Competitividad (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2025202520162025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/381036reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//AYA2011-29754-C03-02http://dx.doi.org/10.3847/2041-8205/822/1/L19Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3810362026-05-22T06:33:51Z
dc.title.none.fl_str_mv HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula
title HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula
spellingShingle HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula
Fang, Xuan
Planetary nebulae: general
Planetary nebulae: individual (NGC 6543)
Stars: winds, outflows
X-rays: ISM
title_short HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula
title_full HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula
title_fullStr HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula
title_full_unstemmed HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula
title_sort HST STIS Observations of the Mixing Layer in the Cat’s Eye Nebula
dc.creator.none.fl_str_mv Fang, Xuan
Guerrero, Martín A.
Toalá, Jesús A.
Chu, You-Hua
Gruendl, Robert A.
author Fang, Xuan
author_facet Fang, Xuan
Guerrero, Martín A.
Toalá, Jesús A.
Chu, You-Hua
Gruendl, Robert A.
author_role author
author2 Guerrero, Martín A.
Toalá, Jesús A.
Chu, You-Hua
Gruendl, Robert A.
author2_role author
author
author
author
dc.contributor.none.fl_str_mv NASA
European Commission
Ministerio de Economía y Competitividad (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Planetary nebulae: general
Planetary nebulae: individual (NGC 6543)
Stars: winds, outflows
X-rays: ISM
topic Planetary nebulae: general
Planetary nebulae: individual (NGC 6543)
Stars: winds, outflows
X-rays: ISM
description Planetary nebulae (PNe) are expected to have a ∼10 K interface layer between the ≥10 K inner hot bubble and the ∼10 K optical nebular shell. The PN structure and evolution, and the X-ray emission, depend critically on the efficiency of the mixing of material at this interface layer. However, neither its location nor its spatial extent have ever been determined. Using high-spatial resolution HST STIS spectroscopic observations of the N v λλ 1239,1243 lines in the Cat's Eye Nebula (NGC 6543), we have detected this interface layer and determined its location, extent, and physical properties for the first time in a PN. We confirm that this interface layer, as revealed by the spatial distribution of the N v λ1239 line emission, is located between the hot bubble and the optical nebular shell. We estimate a thickness of 1.5 × 10 cm and an electron density of ∼200 cm for the mixing layer. With a thermal pressure of ∼2 × 10 yncm, the mixing layer is in pressure equilibrium with the hot bubble and ionized nebular rim of NGC 6543. © 2016. The American Astronomical Society. All rights reserved.
publishDate 2016
dc.date.none.fl_str_mv 2016
2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Postprint
info:eu-repo/semantics/acceptedVersion
format article
status_str acceptedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/381036
url http://hdl.handle.net/10261/381036
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MICINN//AYA2011-29754-C03-02
http://dx.doi.org/10.3847/2041-8205/822/1/L19
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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