Multimission observations of the old nova GK Per during the 2015 outburst

Autores
Zemko, P.; Orio, M.; Luna, Gerardo Juan Manuel; Mukai, K.; Evans, P. A.; Bianchini, A.
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
GK Per, a classical nova of 1901, is thought to undergo variable mass accretion on to a magnetized white dwarf (WD) in an intermediate polar system (IP). We organized a multi-mission observational campaign in the X-ray and ultraviolet (UV) energy ranges during its dwarf nova (DN) outburst in 2015 March-April. Comparing data from quiescence and near outburst, we have found that the maximum plasma temperature decreased from about 26 to 16.2+/-0.4 keV. This is consistent with the previously proposed scenario of increase in mass accretion rate while the inner radius of the magnetically disrupted accretion disc shrinks, thereby lowering the shock temperature. A NuSTAR observation also revealed a high-amplitude WD spin modulation of the very hard X-rays with a single-peaked profile, suggesting an obscuration of the lower accretion pole and an extended shock region on the WD surface. The X-ray spectrum of GK Per measured with the Swift X-Ray Telescope varied on time-scales of days and also showed a gradual increase of the soft X-ray flux below 2 keV, accompanied by a decrease of the hard flux above 2 keV. In the Chandra observation with the High Energy Transmission Gratings, we detected prominent emission lines, especially of Ne, Mg and Si, where the ratios of H-like to He-like transition for each element indicate a much lower temperature than the underlying continuum. We suggest that the X-ray emission in the 0.8-2 keV range originates from the magnetospheric boundary.
Fil: Zemko, P.. Universita Di Padova; Italia
Fil: Orio, M.. Universita Di Padova; Italia
Fil: Luna, Gerardo Juan Manuel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Mukai, K.. National Aeronautics And Space Administration; Estados Unidos
Fil: Evans, P. A.. University of Leicester; Reino Unido
Fil: Bianchini, A.. Universita Di Padova; Italia
Materia
(stars:) novae
cataclysmic variables
stars: individual: GK Per
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/21027
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Multimission observations of the old nova GK Per during the 2015 outburstZemko, P.Orio, M.Luna, Gerardo Juan ManuelMukai, K.Evans, P. A.Bianchini, A.(stars:) novaecataclysmic variablesstars: individual: GK Perhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1GK Per, a classical nova of 1901, is thought to undergo variable mass accretion on to a magnetized white dwarf (WD) in an intermediate polar system (IP). We organized a multi-mission observational campaign in the X-ray and ultraviolet (UV) energy ranges during its dwarf nova (DN) outburst in 2015 March-April. Comparing data from quiescence and near outburst, we have found that the maximum plasma temperature decreased from about 26 to 16.2+/-0.4 keV. This is consistent with the previously proposed scenario of increase in mass accretion rate while the inner radius of the magnetically disrupted accretion disc shrinks, thereby lowering the shock temperature. A NuSTAR observation also revealed a high-amplitude WD spin modulation of the very hard X-rays with a single-peaked profile, suggesting an obscuration of the lower accretion pole and an extended shock region on the WD surface. The X-ray spectrum of GK Per measured with the Swift X-Ray Telescope varied on time-scales of days and also showed a gradual increase of the soft X-ray flux below 2 keV, accompanied by a decrease of the hard flux above 2 keV. In the Chandra observation with the High Energy Transmission Gratings, we detected prominent emission lines, especially of Ne, Mg and Si, where the ratios of H-like to He-like transition for each element indicate a much lower temperature than the underlying continuum. We suggest that the X-ray emission in the 0.8-2 keV range originates from the magnetospheric boundary.Fil: Zemko, P.. Universita Di Padova; ItaliaFil: Orio, M.. Universita Di Padova; ItaliaFil: Luna, Gerardo Juan Manuel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Mukai, K.. National Aeronautics And Space Administration; Estados UnidosFil: Evans, P. A.. University of Leicester; Reino UnidoFil: Bianchini, A.. Universita Di Padova; ItaliaOxford University Press2017-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21027Zemko, P.; Orio, M.; Luna, Gerardo Juan Manuel; Mukai, K.; Evans, P. A.; et al.; Multimission observations of the old nova GK Per during the 2015 outburst; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 469; 1; 7-2017; 476-4910035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx851info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx851info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1705.07707info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-11-05T10:30:12Zoai:ri.conicet.gov.ar:11336/21027instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-11-05 10:30:13.205CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Multimission observations of the old nova GK Per during the 2015 outburst
title Multimission observations of the old nova GK Per during the 2015 outburst
spellingShingle Multimission observations of the old nova GK Per during the 2015 outburst
Zemko, P.
(stars:) novae
cataclysmic variables
stars: individual: GK Per
title_short Multimission observations of the old nova GK Per during the 2015 outburst
title_full Multimission observations of the old nova GK Per during the 2015 outburst
title_fullStr Multimission observations of the old nova GK Per during the 2015 outburst
title_full_unstemmed Multimission observations of the old nova GK Per during the 2015 outburst
title_sort Multimission observations of the old nova GK Per during the 2015 outburst
dc.creator.none.fl_str_mv Zemko, P.
Orio, M.
Luna, Gerardo Juan Manuel
Mukai, K.
Evans, P. A.
Bianchini, A.
author Zemko, P.
author_facet Zemko, P.
Orio, M.
Luna, Gerardo Juan Manuel
Mukai, K.
Evans, P. A.
Bianchini, A.
author_role author
author2 Orio, M.
Luna, Gerardo Juan Manuel
Mukai, K.
Evans, P. A.
Bianchini, A.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv (stars:) novae
cataclysmic variables
stars: individual: GK Per
topic (stars:) novae
cataclysmic variables
stars: individual: GK Per
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv GK Per, a classical nova of 1901, is thought to undergo variable mass accretion on to a magnetized white dwarf (WD) in an intermediate polar system (IP). We organized a multi-mission observational campaign in the X-ray and ultraviolet (UV) energy ranges during its dwarf nova (DN) outburst in 2015 March-April. Comparing data from quiescence and near outburst, we have found that the maximum plasma temperature decreased from about 26 to 16.2+/-0.4 keV. This is consistent with the previously proposed scenario of increase in mass accretion rate while the inner radius of the magnetically disrupted accretion disc shrinks, thereby lowering the shock temperature. A NuSTAR observation also revealed a high-amplitude WD spin modulation of the very hard X-rays with a single-peaked profile, suggesting an obscuration of the lower accretion pole and an extended shock region on the WD surface. The X-ray spectrum of GK Per measured with the Swift X-Ray Telescope varied on time-scales of days and also showed a gradual increase of the soft X-ray flux below 2 keV, accompanied by a decrease of the hard flux above 2 keV. In the Chandra observation with the High Energy Transmission Gratings, we detected prominent emission lines, especially of Ne, Mg and Si, where the ratios of H-like to He-like transition for each element indicate a much lower temperature than the underlying continuum. We suggest that the X-ray emission in the 0.8-2 keV range originates from the magnetospheric boundary.
Fil: Zemko, P.. Universita Di Padova; Italia
Fil: Orio, M.. Universita Di Padova; Italia
Fil: Luna, Gerardo Juan Manuel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Mukai, K.. National Aeronautics And Space Administration; Estados Unidos
Fil: Evans, P. A.. University of Leicester; Reino Unido
Fil: Bianchini, A.. Universita Di Padova; Italia
description GK Per, a classical nova of 1901, is thought to undergo variable mass accretion on to a magnetized white dwarf (WD) in an intermediate polar system (IP). We organized a multi-mission observational campaign in the X-ray and ultraviolet (UV) energy ranges during its dwarf nova (DN) outburst in 2015 March-April. Comparing data from quiescence and near outburst, we have found that the maximum plasma temperature decreased from about 26 to 16.2+/-0.4 keV. This is consistent with the previously proposed scenario of increase in mass accretion rate while the inner radius of the magnetically disrupted accretion disc shrinks, thereby lowering the shock temperature. A NuSTAR observation also revealed a high-amplitude WD spin modulation of the very hard X-rays with a single-peaked profile, suggesting an obscuration of the lower accretion pole and an extended shock region on the WD surface. The X-ray spectrum of GK Per measured with the Swift X-Ray Telescope varied on time-scales of days and also showed a gradual increase of the soft X-ray flux below 2 keV, accompanied by a decrease of the hard flux above 2 keV. In the Chandra observation with the High Energy Transmission Gratings, we detected prominent emission lines, especially of Ne, Mg and Si, where the ratios of H-like to He-like transition for each element indicate a much lower temperature than the underlying continuum. We suggest that the X-ray emission in the 0.8-2 keV range originates from the magnetospheric boundary.
publishDate 2017
dc.date.none.fl_str_mv 2017-07
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/21027
Zemko, P.; Orio, M.; Luna, Gerardo Juan Manuel; Mukai, K.; Evans, P. A.; et al.; Multimission observations of the old nova GK Per during the 2015 outburst; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 469; 1; 7-2017; 476-491
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21027
identifier_str_mv Zemko, P.; Orio, M.; Luna, Gerardo Juan Manuel; Mukai, K.; Evans, P. A.; et al.; Multimission observations of the old nova GK Per during the 2015 outburst; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 469; 1; 7-2017; 476-491
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx851
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx851
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1705.07707
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.087074

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