Aspect angle for interstellar magnetic field in SN 1006

Autores
Petruk, O.; Dubner, Gloria Mabel; Castelletti, Gabriela Marta; Bocchino, F.; Iakubovskyi, D.; Kirsch, M. G. F.; Miceli, M.; Orlando, S.; Telezhinsky, I.
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
A number of important processes taking place around strong shocks in supernova remnants (SNRs) depend on the shock obliquity. The measured synchrotron flux is a function of the aspect angle between interstellar magnetic field (ISMF) and the line of sight. Thus, a model of non-thermal emission from SNRs should account for the orientation of the ambient magnetic field. We develop a new method for the estimation of the aspect angle, based on the comparison between observed and synthesized radio maps of SNRs, making different assumptions about the dependence of electron injection efficiency on the shock obliquity. The method uses the azimuthal profile of radio surface brightness as a probe for orientation of ambient magnetic field because it is almost insensitive to the downstream distribution of magnetic field and emitting electrons. We apply our method to a new radio image of SN 1006 produced on the basis of archival Very Large Array and Parkes data. The image recovers emission from all spatial structures with angular scales from a few arcsec to 15 arcmin. We explore different models of injection efficiency and find the following best-fitting values for the aspect angle of SN 1006: φo = 70o ± 4.2o if the injection is isotropic, φo = 64o ± 2.8o for quasi-perpendicular injection (SNR has an equatorial belt in both cases) and φo = 11o ± 0.8o for quasi-parallel injection (polar-cap model of SNR). In the last case, SN 1006 is expected to have a centrally peaked morphology contrary to what is observed. Therefore, our analysis provides some indication against the quasi-parallel injection model.
Fil: Petruk, O.. Institute for Applied Problems in Mechanics and Mathematics; Ucrania
Fil: Dubner, Gloria Mabel. 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: Castelletti, Gabriela Marta. 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: Bocchino, F.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia
Fil: Iakubovskyi, D.. Bogolyubov Institute for Theoretical Physics; Ucrania
Fil: Kirsch, M. G. F.. European Space Agency; Alemania
Fil: Miceli, M.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia
Fil: Orlando, S.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia
Fil: Telezhinsky, I.. Kiev National Taras Shevchenko University; Ucrania
Materia
ACCELERATION OF PARTICLES
RADIATION MECHANISMS: NON-THERMAL
COSMIC RAYS
ISM: INDIVIDUAL: SN 1006
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:11336/21897
Acceder
id CONICETDig_af95ca222c4eacfaf15a36265dd05053
oai_identifier_str oai:ri.conicet.gov.ar:11336/21897
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Aspect angle for interstellar magnetic field in SN 1006Petruk, O.Dubner, Gloria MabelCastelletti, Gabriela MartaBocchino, F.Iakubovskyi, D.Kirsch, M. G. F.Miceli, M.Orlando, S.Telezhinsky, I.ACCELERATION OF PARTICLESRADIATION MECHANISMS: NON-THERMALCOSMIC RAYSISM: INDIVIDUAL: SN 1006https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1A number of important processes taking place around strong shocks in supernova remnants (SNRs) depend on the shock obliquity. The measured synchrotron flux is a function of the aspect angle between interstellar magnetic field (ISMF) and the line of sight. Thus, a model of non-thermal emission from SNRs should account for the orientation of the ambient magnetic field. We develop a new method for the estimation of the aspect angle, based on the comparison between observed and synthesized radio maps of SNRs, making different assumptions about the dependence of electron injection efficiency on the shock obliquity. The method uses the azimuthal profile of radio surface brightness as a probe for orientation of ambient magnetic field because it is almost insensitive to the downstream distribution of magnetic field and emitting electrons. We apply our method to a new radio image of SN 1006 produced on the basis of archival Very Large Array and Parkes data. The image recovers emission from all spatial structures with angular scales from a few arcsec to 15 arcmin. We explore different models of injection efficiency and find the following best-fitting values for the aspect angle of SN 1006: φo = 70o ± 4.2o if the injection is isotropic, φo = 64o ± 2.8o for quasi-perpendicular injection (SNR has an equatorial belt in both cases) and φo = 11o ± 0.8o for quasi-parallel injection (polar-cap model of SNR). In the last case, SN 1006 is expected to have a centrally peaked morphology contrary to what is observed. Therefore, our analysis provides some indication against the quasi-parallel injection model.Fil: Petruk, O.. Institute for Applied Problems in Mechanics and Mathematics; UcraniaFil: Dubner, Gloria Mabel. 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: Castelletti, Gabriela Marta. 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: Bocchino, F.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; ItaliaFil: Iakubovskyi, D.. Bogolyubov Institute for Theoretical Physics; UcraniaFil: Kirsch, M. G. F.. European Space Agency; AlemaniaFil: Miceli, M.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; ItaliaFil: Orlando, S.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; ItaliaFil: Telezhinsky, I.. Kiev National Taras Shevchenko University; UcraniaOxford University Press2009-12info: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/11336/21897Petruk, O.; Dubner, Gloria Mabel; Castelletti, Gabriela Marta; Bocchino, F.; Iakubovskyi, D.; et al.; Aspect angle for interstellar magnetic field in SN 1006; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 393; 3; 12-2009; 1034-10400035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.14251.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2008.14251.xinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0811.2319info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:01:02Zoai:ri.conicet.gov.ar:11336/21897instacron: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:34982025-10-22 11:01:03.178CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Aspect angle for interstellar magnetic field in SN 1006
title Aspect angle for interstellar magnetic field in SN 1006
spellingShingle Aspect angle for interstellar magnetic field in SN 1006
Petruk, O.
ACCELERATION OF PARTICLES
RADIATION MECHANISMS: NON-THERMAL
COSMIC RAYS
ISM: INDIVIDUAL: SN 1006
title_short Aspect angle for interstellar magnetic field in SN 1006
title_full Aspect angle for interstellar magnetic field in SN 1006
title_fullStr Aspect angle for interstellar magnetic field in SN 1006
title_full_unstemmed Aspect angle for interstellar magnetic field in SN 1006
title_sort Aspect angle for interstellar magnetic field in SN 1006
dc.creator.none.fl_str_mv Petruk, O.
Dubner, Gloria Mabel
Castelletti, Gabriela Marta
Bocchino, F.
Iakubovskyi, D.
Kirsch, M. G. F.
Miceli, M.
Orlando, S.
Telezhinsky, I.
author Petruk, O.
author_facet Petruk, O.
Dubner, Gloria Mabel
Castelletti, Gabriela Marta
Bocchino, F.
Iakubovskyi, D.
Kirsch, M. G. F.
Miceli, M.
Orlando, S.
Telezhinsky, I.
author_role author
author2 Dubner, Gloria Mabel
Castelletti, Gabriela Marta
Bocchino, F.
Iakubovskyi, D.
Kirsch, M. G. F.
Miceli, M.
Orlando, S.
Telezhinsky, I.
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ACCELERATION OF PARTICLES
RADIATION MECHANISMS: NON-THERMAL
COSMIC RAYS
ISM: INDIVIDUAL: SN 1006
topic ACCELERATION OF PARTICLES
RADIATION MECHANISMS: NON-THERMAL
COSMIC RAYS
ISM: INDIVIDUAL: SN 1006
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv A number of important processes taking place around strong shocks in supernova remnants (SNRs) depend on the shock obliquity. The measured synchrotron flux is a function of the aspect angle between interstellar magnetic field (ISMF) and the line of sight. Thus, a model of non-thermal emission from SNRs should account for the orientation of the ambient magnetic field. We develop a new method for the estimation of the aspect angle, based on the comparison between observed and synthesized radio maps of SNRs, making different assumptions about the dependence of electron injection efficiency on the shock obliquity. The method uses the azimuthal profile of radio surface brightness as a probe for orientation of ambient magnetic field because it is almost insensitive to the downstream distribution of magnetic field and emitting electrons. We apply our method to a new radio image of SN 1006 produced on the basis of archival Very Large Array and Parkes data. The image recovers emission from all spatial structures with angular scales from a few arcsec to 15 arcmin. We explore different models of injection efficiency and find the following best-fitting values for the aspect angle of SN 1006: φo = 70o ± 4.2o if the injection is isotropic, φo = 64o ± 2.8o for quasi-perpendicular injection (SNR has an equatorial belt in both cases) and φo = 11o ± 0.8o for quasi-parallel injection (polar-cap model of SNR). In the last case, SN 1006 is expected to have a centrally peaked morphology contrary to what is observed. Therefore, our analysis provides some indication against the quasi-parallel injection model.
Fil: Petruk, O.. Institute for Applied Problems in Mechanics and Mathematics; Ucrania
Fil: Dubner, Gloria Mabel. 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: Castelletti, Gabriela Marta. 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: Bocchino, F.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia
Fil: Iakubovskyi, D.. Bogolyubov Institute for Theoretical Physics; Ucrania
Fil: Kirsch, M. G. F.. European Space Agency; Alemania
Fil: Miceli, M.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia
Fil: Orlando, S.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia
Fil: Telezhinsky, I.. Kiev National Taras Shevchenko University; Ucrania
description A number of important processes taking place around strong shocks in supernova remnants (SNRs) depend on the shock obliquity. The measured synchrotron flux is a function of the aspect angle between interstellar magnetic field (ISMF) and the line of sight. Thus, a model of non-thermal emission from SNRs should account for the orientation of the ambient magnetic field. We develop a new method for the estimation of the aspect angle, based on the comparison between observed and synthesized radio maps of SNRs, making different assumptions about the dependence of electron injection efficiency on the shock obliquity. The method uses the azimuthal profile of radio surface brightness as a probe for orientation of ambient magnetic field because it is almost insensitive to the downstream distribution of magnetic field and emitting electrons. We apply our method to a new radio image of SN 1006 produced on the basis of archival Very Large Array and Parkes data. The image recovers emission from all spatial structures with angular scales from a few arcsec to 15 arcmin. We explore different models of injection efficiency and find the following best-fitting values for the aspect angle of SN 1006: φo = 70o ± 4.2o if the injection is isotropic, φo = 64o ± 2.8o for quasi-perpendicular injection (SNR has an equatorial belt in both cases) and φo = 11o ± 0.8o for quasi-parallel injection (polar-cap model of SNR). In the last case, SN 1006 is expected to have a centrally peaked morphology contrary to what is observed. Therefore, our analysis provides some indication against the quasi-parallel injection model.
publishDate 2009
dc.date.none.fl_str_mv 2009-12
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/11336/21897
Petruk, O.; Dubner, Gloria Mabel; Castelletti, Gabriela Marta; Bocchino, F.; Iakubovskyi, D.; et al.; Aspect angle for interstellar magnetic field in SN 1006; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 393; 3; 12-2009; 1034-1040
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21897
identifier_str_mv Petruk, O.; Dubner, Gloria Mabel; Castelletti, Gabriela Marta; Bocchino, F.; Iakubovskyi, D.; et al.; Aspect angle for interstellar magnetic field in SN 1006; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 393; 3; 12-2009; 1034-1040
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/doi/10.1111/j.1365-2966.2008.14251.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2008.14251.x
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0811.2319
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 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
_version_ 1846781185688076288
score 12.982451

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