Stellar wind structures in the eclipsing binary system IGR J18027-2016

Autores
Fogantini, Federico Adrián; García, Federico; Combi, Jorge Ariel; Chaty, Sylvain
Año de publicación
2021
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. IGR J18027-2016 is an obscured high-mass X-ray binary formed by a neutron star accreting from the wind of a supergiant companion with a ∼4.57 d orbital period. The source shows an asymmetric eclipse profile that remained stable across several years. Aims. We aim to investigate the geometrical and physical properties of stellar wind structures formed by the interaction between the compact object and the supergiant star. Methods. In this work we analysed the temporal and spectral evolution of this source along its orbit using six archival XMM-Newton observations and the accumulated Swift/BAT hard X-ray light curve. Results. The XMM-Newton light curves show that the source hardens during the ingress and egress of the eclipse, in accordance with the asymmetric profile seen in Swift/BAT data. A reduced pulse modulation is observed on the ingress to the eclipse. We modelled XMM-Newton spectra by means of a thermally Comptonized continuum (NTHCOMP), adding two Gaussian emission lines corresponding to Fe Kα and Fe Kβ. We included two absorption components to account for the interstellar and intrinsic media. We found that the local absorption column outside the eclipse fluctuates uniformly around ∼6 × 1022 cm-2, whereas when the source enters and leaves the eclipse the column increases by a factor of 3, reaching values up to ∼35 and ∼15 × 1022 cm-2, respectively. Conclusions. Combining the physical properties derived from the spectral analysis, we propose a scenario in which, primarily, a photo-ionisation wake and, secondarily, an accretion wake are responsible for the orbital evolution of the absorption column, continuum emission, and variability seen at the Fe-line complex.
Fil: Fogantini, Federico Adrián. Universidad Nacional de La Plata; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Combi, Jorge Ariel. Universite Paris Saclay; Francia
Fil: Chaty, Sylvain. University Of Groningen; Países Bajos
Materia
STARS: NEUTRON
X-RAYS: BINARIES
X-RAYS: INDIVIDUALS: IGR J18027-2016
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:11336/135295
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/135295
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Stellar wind structures in the eclipsing binary system IGR J18027-2016Fogantini, Federico AdriánGarcía, FedericoCombi, Jorge ArielChaty, SylvainSTARS: NEUTRONX-RAYS: BINARIESX-RAYS: INDIVIDUALS: IGR J18027-2016https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. IGR J18027-2016 is an obscured high-mass X-ray binary formed by a neutron star accreting from the wind of a supergiant companion with a ∼4.57 d orbital period. The source shows an asymmetric eclipse profile that remained stable across several years. Aims. We aim to investigate the geometrical and physical properties of stellar wind structures formed by the interaction between the compact object and the supergiant star. Methods. In this work we analysed the temporal and spectral evolution of this source along its orbit using six archival XMM-Newton observations and the accumulated Swift/BAT hard X-ray light curve. Results. The XMM-Newton light curves show that the source hardens during the ingress and egress of the eclipse, in accordance with the asymmetric profile seen in Swift/BAT data. A reduced pulse modulation is observed on the ingress to the eclipse. We modelled XMM-Newton spectra by means of a thermally Comptonized continuum (NTHCOMP), adding two Gaussian emission lines corresponding to Fe Kα and Fe Kβ. We included two absorption components to account for the interstellar and intrinsic media. We found that the local absorption column outside the eclipse fluctuates uniformly around ∼6 × 1022 cm-2, whereas when the source enters and leaves the eclipse the column increases by a factor of 3, reaching values up to ∼35 and ∼15 × 1022 cm-2, respectively. Conclusions. Combining the physical properties derived from the spectral analysis, we propose a scenario in which, primarily, a photo-ionisation wake and, secondarily, an accretion wake are responsible for the orbital evolution of the absorption column, continuum emission, and variability seen at the Fe-line complex.Fil: Fogantini, Federico Adrián. Universidad Nacional de La Plata; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Combi, Jorge Ariel. Universite Paris Saclay; FranciaFil: Chaty, Sylvain. University Of Groningen; Países BajosEDP Sciences2021-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/135295Fogantini, Federico Adrián; García, Federico; Combi, Jorge Ariel; Chaty, Sylvain; Stellar wind structures in the eclipsing binary system IGR J18027-2016; EDP Sciences; Astronomy and Astrophysics; 647; 3-2021; 75-870004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202039088info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039088info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:23:40Zoai:ri.conicet.gov.ar:11336/135295instacron: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:34982025-10-15 15:23:40.473CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Stellar wind structures in the eclipsing binary system IGR J18027-2016
title Stellar wind structures in the eclipsing binary system IGR J18027-2016
spellingShingle Stellar wind structures in the eclipsing binary system IGR J18027-2016
Fogantini, Federico Adrián
STARS: NEUTRON
X-RAYS: BINARIES
X-RAYS: INDIVIDUALS: IGR J18027-2016
title_short Stellar wind structures in the eclipsing binary system IGR J18027-2016
title_full Stellar wind structures in the eclipsing binary system IGR J18027-2016
title_fullStr Stellar wind structures in the eclipsing binary system IGR J18027-2016
title_full_unstemmed Stellar wind structures in the eclipsing binary system IGR J18027-2016
title_sort Stellar wind structures in the eclipsing binary system IGR J18027-2016
dc.creator.none.fl_str_mv Fogantini, Federico Adrián
García, Federico
Combi, Jorge Ariel
Chaty, Sylvain
author Fogantini, Federico Adrián
author_facet Fogantini, Federico Adrián
García, Federico
Combi, Jorge Ariel
Chaty, Sylvain
author_role author
author2 García, Federico
Combi, Jorge Ariel
Chaty, Sylvain
author2_role author
author
author
dc.subject.none.fl_str_mv STARS: NEUTRON
X-RAYS: BINARIES
X-RAYS: INDIVIDUALS: IGR J18027-2016
topic STARS: NEUTRON
X-RAYS: BINARIES
X-RAYS: INDIVIDUALS: IGR J18027-2016
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. IGR J18027-2016 is an obscured high-mass X-ray binary formed by a neutron star accreting from the wind of a supergiant companion with a ∼4.57 d orbital period. The source shows an asymmetric eclipse profile that remained stable across several years. Aims. We aim to investigate the geometrical and physical properties of stellar wind structures formed by the interaction between the compact object and the supergiant star. Methods. In this work we analysed the temporal and spectral evolution of this source along its orbit using six archival XMM-Newton observations and the accumulated Swift/BAT hard X-ray light curve. Results. The XMM-Newton light curves show that the source hardens during the ingress and egress of the eclipse, in accordance with the asymmetric profile seen in Swift/BAT data. A reduced pulse modulation is observed on the ingress to the eclipse. We modelled XMM-Newton spectra by means of a thermally Comptonized continuum (NTHCOMP), adding two Gaussian emission lines corresponding to Fe Kα and Fe Kβ. We included two absorption components to account for the interstellar and intrinsic media. We found that the local absorption column outside the eclipse fluctuates uniformly around ∼6 × 1022 cm-2, whereas when the source enters and leaves the eclipse the column increases by a factor of 3, reaching values up to ∼35 and ∼15 × 1022 cm-2, respectively. Conclusions. Combining the physical properties derived from the spectral analysis, we propose a scenario in which, primarily, a photo-ionisation wake and, secondarily, an accretion wake are responsible for the orbital evolution of the absorption column, continuum emission, and variability seen at the Fe-line complex.
Fil: Fogantini, Federico Adrián. Universidad Nacional de La Plata; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Combi, Jorge Ariel. Universite Paris Saclay; Francia
Fil: Chaty, Sylvain. University Of Groningen; Países Bajos
description Context. IGR J18027-2016 is an obscured high-mass X-ray binary formed by a neutron star accreting from the wind of a supergiant companion with a ∼4.57 d orbital period. The source shows an asymmetric eclipse profile that remained stable across several years. Aims. We aim to investigate the geometrical and physical properties of stellar wind structures formed by the interaction between the compact object and the supergiant star. Methods. In this work we analysed the temporal and spectral evolution of this source along its orbit using six archival XMM-Newton observations and the accumulated Swift/BAT hard X-ray light curve. Results. The XMM-Newton light curves show that the source hardens during the ingress and egress of the eclipse, in accordance with the asymmetric profile seen in Swift/BAT data. A reduced pulse modulation is observed on the ingress to the eclipse. We modelled XMM-Newton spectra by means of a thermally Comptonized continuum (NTHCOMP), adding two Gaussian emission lines corresponding to Fe Kα and Fe Kβ. We included two absorption components to account for the interstellar and intrinsic media. We found that the local absorption column outside the eclipse fluctuates uniformly around ∼6 × 1022 cm-2, whereas when the source enters and leaves the eclipse the column increases by a factor of 3, reaching values up to ∼35 and ∼15 × 1022 cm-2, respectively. Conclusions. Combining the physical properties derived from the spectral analysis, we propose a scenario in which, primarily, a photo-ionisation wake and, secondarily, an accretion wake are responsible for the orbital evolution of the absorption column, continuum emission, and variability seen at the Fe-line complex.
publishDate 2021
dc.date.none.fl_str_mv 2021-03
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/11336/135295
Fogantini, Federico Adrián; García, Federico; Combi, Jorge Ariel; Chaty, Sylvain; Stellar wind structures in the eclipsing binary system IGR J18027-2016; EDP Sciences; Astronomy and Astrophysics; 647; 3-2021; 75-87
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/135295
identifier_str_mv Fogantini, Federico Adrián; García, Federico; Combi, Jorge Ariel; Chaty, Sylvain; Stellar wind structures in the eclipsing binary system IGR J18027-2016; EDP Sciences; Astronomy and Astrophysics; 647; 3-2021; 75-87
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/10.1051/0004-6361/202039088
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039088
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
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 13.22299

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