Rebirth of x-ray emission from the born-again planetary nebula A30

The planetary nebula A30 is believed to have undergone a very late thermal pulse resulting in the ejection of knots of hydrogen-poor material. Using multi-epoch Hubble Space Telescope images, we have detected the angular expansion of these knots and derived an age of 850+280 - 150 yr. To investigate...

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Autores: Guerrero, Martín A., Ruiz, N., Hamann, W. -R., Chu, Y. -H., Todt, H., Schönberner, D., Oskinova, L., Gruendl, R. A., Steffen, M., Blair, W. P., Toalá, Jesús A.
Formato: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2012
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/414300
Acesso em linha:http://hdl.handle.net/10261/414300
Access Level:acceso abierto
Palavra-chave:Planetary nebulae: general
Planetary nebulae: individual (A30)
Stars: winds, outflows
X-rays: ISM
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spelling Rebirth of x-ray emission from the born-again planetary nebula A30Guerrero, Martín A.Ruiz, N.Hamann, W. -R.Chu, Y. -H.Todt, H.Schönberner, D.Oskinova, L.Gruendl, R. A.Steffen, M.Blair, W. P.Toalá, Jesús A.Planetary nebulae: generalPlanetary nebulae: individual (A30)Stars: winds, outflowsX-rays: ISMThe planetary nebula A30 is believed to have undergone a very late thermal pulse resulting in the ejection of knots of hydrogen-poor material. Using multi-epoch Hubble Space Telescope images, we have detected the angular expansion of these knots and derived an age of 850+280 - 150 yr. To investigate the spectral and spatial properties of the soft X-ray emission detected by ROSAT, we have obtained Chandra and XMM-Newton deep observations of A30. The X-ray emission from A30 can be separated into two components: a point source at the central star and diffuse emission associated with the hydrogen-poor knots and the cloverleaf structure inside the nebular shell. To help us assess the role of the current stellar wind in powering this X-ray emission, we have determined the stellar parameters and wind properties of the central star of A30 using a non-LTE model fit to its optical and UV spectra. The spatial distribution and spectral properties of the diffuse X-ray emission are highly suggestive that it is generated by the post-born-again and present fast stellar winds interacting with the hydrogen-poor ejecta of the born-again event. This emission can be attributed to shock-heated plasma, as the hydrogen-poor knots are ablated by the stellar winds, under which circumstances the efficient mass loading of the present fast stellar wind raises its density and damps its velocity to produce the observed diffuse soft X-rays. Charge transfer reactions between the ions of the stellar winds and material of the born-again ejecta have also been considered as a possible mechanism for the production of diffuse X-ray emission, and upper limits on the expected X-ray production by this mechanism have been derived. The origin of the X-ray emission from the central star of A30 is puzzling: shocks in the present fast stellar wind and photospheric emission can be ruled out, while the development of a new, compact hot bubble confining the fast stellar wind seems implausible. © 2012. The American Astronomical Society. All rights reserved.M.A.G., N.R., and J.T. are partially funded by grants AYA 2008-01934 and AYA2011-29754-C03-02 of the Spanish MICINN (Ministerio de Ciencia e Innovaci´on) and MEC (Min- isterio de Econom´ıa y Competitividad). Y.-H.C. and R.A.G. acknowledge the support of NASA grants NNX09AU32G and SAO GO01-12029X. Funding for this research has been pro- vided by DLR grant 50 OR 1101 (LMO). We are grateful to an anonymous referee for pointing out the importance of charge transfer on dust and for detailed comments on charge trans- fer that significantly improved the manuscript. We are very grateful to Ralf Napiwotzki for providing us with the optical high-dispersion spectra of the central star of A30 and to Sarah J. Arthur for helpful discussion on charge transfer to dust and ions.Peer reviewedIOP PublishingMinisterio de Ciencia e Innovación (España)Ministerio de Economía y Competitividad (España)NASAConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202620262012info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/414300reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//AYA2008-01934info:eu-repo/grantAgreement/MINECO//AYA2011-29754-C03-02http://dx.doi.org/10.1088/0004-637X/755/2/129Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/4143002026-05-22T06:33:51Z
dc.title.none.fl_str_mv Rebirth of x-ray emission from the born-again planetary nebula A30
title Rebirth of x-ray emission from the born-again planetary nebula A30
spellingShingle Rebirth of x-ray emission from the born-again planetary nebula A30
Guerrero, Martín A.
Planetary nebulae: general
Planetary nebulae: individual (A30)
Stars: winds, outflows
X-rays: ISM
title_short Rebirth of x-ray emission from the born-again planetary nebula A30
title_full Rebirth of x-ray emission from the born-again planetary nebula A30
title_fullStr Rebirth of x-ray emission from the born-again planetary nebula A30
title_full_unstemmed Rebirth of x-ray emission from the born-again planetary nebula A30
title_sort Rebirth of x-ray emission from the born-again planetary nebula A30
dc.creator.none.fl_str_mv Guerrero, Martín A.
Ruiz, N.
Hamann, W. -R.
Chu, Y. -H.
Todt, H.
Schönberner, D.
Oskinova, L.
Gruendl, R. A.
Steffen, M.
Blair, W. P.
Toalá, Jesús A.
author Guerrero, Martín A.
author_facet Guerrero, Martín A.
Ruiz, N.
Hamann, W. -R.
Chu, Y. -H.
Todt, H.
Schönberner, D.
Oskinova, L.
Gruendl, R. A.
Steffen, M.
Blair, W. P.
Toalá, Jesús A.
author_role author
author2 Ruiz, N.
Hamann, W. -R.
Chu, Y. -H.
Todt, H.
Schönberner, D.
Oskinova, L.
Gruendl, R. A.
Steffen, M.
Blair, W. P.
Toalá, Jesús A.
author2_role author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
Ministerio de Economía y Competitividad (España)
NASA
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Planetary nebulae: general
Planetary nebulae: individual (A30)
Stars: winds, outflows
X-rays: ISM
topic Planetary nebulae: general
Planetary nebulae: individual (A30)
Stars: winds, outflows
X-rays: ISM
description The planetary nebula A30 is believed to have undergone a very late thermal pulse resulting in the ejection of knots of hydrogen-poor material. Using multi-epoch Hubble Space Telescope images, we have detected the angular expansion of these knots and derived an age of 850+280 - 150 yr. To investigate the spectral and spatial properties of the soft X-ray emission detected by ROSAT, we have obtained Chandra and XMM-Newton deep observations of A30. The X-ray emission from A30 can be separated into two components: a point source at the central star and diffuse emission associated with the hydrogen-poor knots and the cloverleaf structure inside the nebular shell. To help us assess the role of the current stellar wind in powering this X-ray emission, we have determined the stellar parameters and wind properties of the central star of A30 using a non-LTE model fit to its optical and UV spectra. The spatial distribution and spectral properties of the diffuse X-ray emission are highly suggestive that it is generated by the post-born-again and present fast stellar winds interacting with the hydrogen-poor ejecta of the born-again event. This emission can be attributed to shock-heated plasma, as the hydrogen-poor knots are ablated by the stellar winds, under which circumstances the efficient mass loading of the present fast stellar wind raises its density and damps its velocity to produce the observed diffuse soft X-rays. Charge transfer reactions between the ions of the stellar winds and material of the born-again ejecta have also been considered as a possible mechanism for the production of diffuse X-ray emission, and upper limits on the expected X-ray production by this mechanism have been derived. The origin of the X-ray emission from the central star of A30 is puzzling: shocks in the present fast stellar wind and photospheric emission can be ruled out, while the development of a new, compact hot bubble confining the fast stellar wind seems implausible. © 2012. The American Astronomical Society. All rights reserved.
publishDate 2012
dc.date.none.fl_str_mv 2012
2026
2026
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/10261/414300
url http://hdl.handle.net/10261/414300
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MICINN//AYA2008-01934
info:eu-repo/grantAgreement/MINECO//AYA2011-29754-C03-02
http://dx.doi.org/10.1088/0004-637X/755/2/129
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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score 15,811543

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