Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations

Autores
de Jesus Lima, Isabel; Luna, Gerardo Juan Manuel; Mukai, K.; Oliveira, A. S.; Sokoloski, J. L.; Walter, F. M.; Palivanas, N.; Nuñez, Natalia Edith; Souza, R. R.; Araujo, R. A. N.
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
White dwarf symbiotic binaries are detected in X-rays with luminosities in the range of 1030–1034 ergs s−1. Their X-ray emission ariseseither from the accretion disk boundary layer, from a region where the winds from both components collide, or from nuclear burningon the surface of the white dwarf (WD). In our continuous effort to identify X-ray-emitting symbiotic stars, we studied four systemsusing observations from the Neil Gehrels Swift Observatory and XMM-Newton satellites in X-rays and from Transiting ExoplanetSurvey Satellite (TESS) in the optical. The X-ray spectra were fit with absorbed optically thin thermal plasma models that are eithersingle- or multitemperature with kT < 8 keV for all targets. Based on the characteristics of their X-ray spectra, we classified BD Camas possible β-type, V1261 Ori and CD −27 8661 as δ-type, and confirmed NQ Gem as β/δ-type. The δ-type X-ray emission most likelyarises from the boundary layer of the accretion disk, while in the case of BD Cam, its mostly soft emission originates from shocks,possibly between the red giant and WD and disk winds. In general, we find that the observed X-ray emission is powered by accretionat a low accretion rate of about 10−11 M yr−1. The low ratio of X-ray to optical luminosities, however indicates that the accretion-diskboundary layer is mostly optically thick and tends to emit in the far or extreme UV. The detection of flickering in optical data providesevidence of the existence of an accretion disk.
Fil: de Jesus Lima, Isabel. Consejo Nacional de Investigaciones 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. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales; Argentina. Universidade Estadual Paulista Julio de Mesquita Filho; Brasil
Fil: Luna, Gerardo Juan Manuel. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Hurlingham; Argentina
Fil: Mukai, K.. National Aeronautics and Space Administration; Estados Unidos. University of Maryland; Estados Unidos
Fil: Oliveira, A. S.. Universidade do Vale do Paraíba; Brasil
Fil: Sokoloski, J. L.. Columbia University; Estados Unidos
Fil: Walter, F. M.. State University of New York; Estados Unidos
Fil: Palivanas, N.. Universidade do Vale do Paraíba; Brasil
Fil: Nuñez, Natalia Edith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales; Argentina
Fil: Souza, R. R.. Universidade Estadual Paulista Julio de Mesquita Filho; Brasil
Fil: Araujo, R. A. N.. Instituto de Ciencia y Tecnologia ; Universidade Estadual Paulista Julio de Mesquita Filho;
Materia
BINARIES: SYMBIOTIC
STARS: INDIVIDUAL: BD CAM
STARS: INDIVIDUAL: V1261 ORI
STARS: INDIVIDUAL: NQ GEM
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/244428
Acceder
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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observationsde Jesus Lima, IsabelLuna, Gerardo Juan ManuelMukai, K.Oliveira, A. S.Sokoloski, J. L.Walter, F. M.Palivanas, N.Nuñez, Natalia EdithSouza, R. R.Araujo, R. A. N.BINARIES: SYMBIOTICSTARS: INDIVIDUAL: BD CAMSTARS: INDIVIDUAL: V1261 ORISTARS: INDIVIDUAL: NQ GEMhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1White dwarf symbiotic binaries are detected in X-rays with luminosities in the range of 1030–1034 ergs s−1. Their X-ray emission ariseseither from the accretion disk boundary layer, from a region where the winds from both components collide, or from nuclear burningon the surface of the white dwarf (WD). In our continuous effort to identify X-ray-emitting symbiotic stars, we studied four systemsusing observations from the Neil Gehrels Swift Observatory and XMM-Newton satellites in X-rays and from Transiting ExoplanetSurvey Satellite (TESS) in the optical. The X-ray spectra were fit with absorbed optically thin thermal plasma models that are eithersingle- or multitemperature with kT < 8 keV for all targets. Based on the characteristics of their X-ray spectra, we classified BD Camas possible β-type, V1261 Ori and CD −27 8661 as δ-type, and confirmed NQ Gem as β/δ-type. The δ-type X-ray emission most likelyarises from the boundary layer of the accretion disk, while in the case of BD Cam, its mostly soft emission originates from shocks,possibly between the red giant and WD and disk winds. In general, we find that the observed X-ray emission is powered by accretionat a low accretion rate of about 10−11 M yr−1. The low ratio of X-ray to optical luminosities, however indicates that the accretion-diskboundary layer is mostly optically thick and tends to emit in the far or extreme UV. The detection of flickering in optical data providesevidence of the existence of an accretion disk.Fil: de Jesus Lima, Isabel. Consejo Nacional de Investigaciones 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. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales; Argentina. Universidade Estadual Paulista Julio de Mesquita Filho; BrasilFil: Luna, Gerardo Juan Manuel. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Hurlingham; ArgentinaFil: Mukai, K.. National Aeronautics and Space Administration; Estados Unidos. University of Maryland; Estados UnidosFil: Oliveira, A. S.. Universidade do Vale do Paraíba; BrasilFil: Sokoloski, J. L.. Columbia University; Estados UnidosFil: Walter, F. M.. State University of New York; Estados UnidosFil: Palivanas, N.. Universidade do Vale do Paraíba; BrasilFil: Nuñez, Natalia Edith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales; ArgentinaFil: Souza, R. R.. Universidade Estadual Paulista Julio de Mesquita Filho; BrasilFil: Araujo, R. A. N.. Instituto de Ciencia y Tecnologia ; Universidade Estadual Paulista Julio de Mesquita Filho;EDP Sciences2024-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/244428de Jesus Lima, Isabel; Luna, Gerardo Juan Manuel; Mukai, K.; Oliveira, A. S.; Sokoloski, J. L.; et al.; Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations; EDP Sciences; Astronomy and Astrophysics; 689; 9-2024; 1-180004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202449913info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202449913info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:37:30Zoai:ri.conicet.gov.ar:11336/244428instacron: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:34982025-09-29 10:37:30.738CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations
title Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations
spellingShingle Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations
de Jesus Lima, Isabel
BINARIES: SYMBIOTIC
STARS: INDIVIDUAL: BD CAM
STARS: INDIVIDUAL: V1261 ORI
STARS: INDIVIDUAL: NQ GEM
title_short Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations
title_full Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations
title_fullStr Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations
title_full_unstemmed Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations
title_sort Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations
dc.creator.none.fl_str_mv de Jesus Lima, Isabel
Luna, Gerardo Juan Manuel
Mukai, K.
Oliveira, A. S.
Sokoloski, J. L.
Walter, F. M.
Palivanas, N.
Nuñez, Natalia Edith
Souza, R. R.
Araujo, R. A. N.
author de Jesus Lima, Isabel
author_facet de Jesus Lima, Isabel
Luna, Gerardo Juan Manuel
Mukai, K.
Oliveira, A. S.
Sokoloski, J. L.
Walter, F. M.
Palivanas, N.
Nuñez, Natalia Edith
Souza, R. R.
Araujo, R. A. N.
author_role author
author2 Luna, Gerardo Juan Manuel
Mukai, K.
Oliveira, A. S.
Sokoloski, J. L.
Walter, F. M.
Palivanas, N.
Nuñez, Natalia Edith
Souza, R. R.
Araujo, R. A. N.
author2_role author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv BINARIES: SYMBIOTIC
STARS: INDIVIDUAL: BD CAM
STARS: INDIVIDUAL: V1261 ORI
STARS: INDIVIDUAL: NQ GEM
topic BINARIES: SYMBIOTIC
STARS: INDIVIDUAL: BD CAM
STARS: INDIVIDUAL: V1261 ORI
STARS: INDIVIDUAL: NQ GEM
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv White dwarf symbiotic binaries are detected in X-rays with luminosities in the range of 1030–1034 ergs s−1. Their X-ray emission ariseseither from the accretion disk boundary layer, from a region where the winds from both components collide, or from nuclear burningon the surface of the white dwarf (WD). In our continuous effort to identify X-ray-emitting symbiotic stars, we studied four systemsusing observations from the Neil Gehrels Swift Observatory and XMM-Newton satellites in X-rays and from Transiting ExoplanetSurvey Satellite (TESS) in the optical. The X-ray spectra were fit with absorbed optically thin thermal plasma models that are eithersingle- or multitemperature with kT < 8 keV for all targets. Based on the characteristics of their X-ray spectra, we classified BD Camas possible β-type, V1261 Ori and CD −27 8661 as δ-type, and confirmed NQ Gem as β/δ-type. The δ-type X-ray emission most likelyarises from the boundary layer of the accretion disk, while in the case of BD Cam, its mostly soft emission originates from shocks,possibly between the red giant and WD and disk winds. In general, we find that the observed X-ray emission is powered by accretionat a low accretion rate of about 10−11 M yr−1. The low ratio of X-ray to optical luminosities, however indicates that the accretion-diskboundary layer is mostly optically thick and tends to emit in the far or extreme UV. The detection of flickering in optical data providesevidence of the existence of an accretion disk.
Fil: de Jesus Lima, Isabel. Consejo Nacional de Investigaciones 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. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales; Argentina. Universidade Estadual Paulista Julio de Mesquita Filho; Brasil
Fil: Luna, Gerardo Juan Manuel. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Hurlingham; Argentina
Fil: Mukai, K.. National Aeronautics and Space Administration; Estados Unidos. University of Maryland; Estados Unidos
Fil: Oliveira, A. S.. Universidade do Vale do Paraíba; Brasil
Fil: Sokoloski, J. L.. Columbia University; Estados Unidos
Fil: Walter, F. M.. State University of New York; Estados Unidos
Fil: Palivanas, N.. Universidade do Vale do Paraíba; Brasil
Fil: Nuñez, Natalia Edith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales; Argentina
Fil: Souza, R. R.. Universidade Estadual Paulista Julio de Mesquita Filho; Brasil
Fil: Araujo, R. A. N.. Instituto de Ciencia y Tecnologia ; Universidade Estadual Paulista Julio de Mesquita Filho;
description White dwarf symbiotic binaries are detected in X-rays with luminosities in the range of 1030–1034 ergs s−1. Their X-ray emission ariseseither from the accretion disk boundary layer, from a region where the winds from both components collide, or from nuclear burningon the surface of the white dwarf (WD). In our continuous effort to identify X-ray-emitting symbiotic stars, we studied four systemsusing observations from the Neil Gehrels Swift Observatory and XMM-Newton satellites in X-rays and from Transiting ExoplanetSurvey Satellite (TESS) in the optical. The X-ray spectra were fit with absorbed optically thin thermal plasma models that are eithersingle- or multitemperature with kT < 8 keV for all targets. Based on the characteristics of their X-ray spectra, we classified BD Camas possible β-type, V1261 Ori and CD −27 8661 as δ-type, and confirmed NQ Gem as β/δ-type. The δ-type X-ray emission most likelyarises from the boundary layer of the accretion disk, while in the case of BD Cam, its mostly soft emission originates from shocks,possibly between the red giant and WD and disk winds. In general, we find that the observed X-ray emission is powered by accretionat a low accretion rate of about 10−11 M yr−1. The low ratio of X-ray to optical luminosities, however indicates that the accretion-diskboundary layer is mostly optically thick and tends to emit in the far or extreme UV. The detection of flickering in optical data providesevidence of the existence of an accretion disk.
publishDate 2024
dc.date.none.fl_str_mv 2024-09
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/11336/244428
de Jesus Lima, Isabel; Luna, Gerardo Juan Manuel; Mukai, K.; Oliveira, A. S.; Sokoloski, J. L.; et al.; Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations; EDP Sciences; Astronomy and Astrophysics; 689; 9-2024; 1-18
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/244428
identifier_str_mv de Jesus Lima, Isabel; Luna, Gerardo Juan Manuel; Mukai, K.; Oliveira, A. S.; Sokoloski, J. L.; et al.; Symbiotic stars in X-rays IV. XMM-Newton, Swift, and TESS observations; EDP Sciences; Astronomy and Astrophysics; 689; 9-2024; 1-18
0004-6361
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://www.aanda.org/10.1051/0004-6361/202449913
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202449913
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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 13.070432

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