Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?

Autores
Butt, Yousaf M.; Torres, Diego F.; Combi, Jorge Ariel; Dame, Thomas M.; Romero, Gustavo Esteban
Año de publicación
2001
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The nonthermal supernova remnant (SNR) RX J1713.7-3946 has recently been shown to be a site of cosmic-ray (CR) electron acceleration to TeV energies. Here we present evidence that this remnant is also accelerating CR nuclei. Such energetic nuclei can interact with ambient interstellar gas to produce high-energy gamma rays via the decay of neutral pions. We associate the unidentified EGRET GeV gamma-ray source, 3EG J1714-3857, with a very massive (~3×105 Msolar) and dense (~500 nucleons cm-3) molecular cloud interacting with SNR RX J1713.7-3946. Direct evidence for such interaction is provided by observations of the lowest two rotational transitions of CO molecules in the cloud; as in other clear cases of interaction, the CO(J=2-->1)/CO(J=1-->0) ratio is significantly enhanced. Since the cloud is of low radio and X-ray brightness, electrons cannot be responsible for the bulk of the GeV emission there. A picture thus emerges in which both electrons and nuclei are being accelerated by the SNR: whereas the relativistic electrons dominate the local nonthermal radio, X-ray, and TeV emission, the shock-accelerated CR protons and ions (hadrons) are exposed through their interactions in the adjacent massive cloud, leading to the observed GeV emission via the gamma decay of neutral pions.
Fil: Butt, Yousaf M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Torres, Diego F.. University of Princeton; Estados Unidos. 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. 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: Dame, Thomas M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Romero, Gustavo Esteban. 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
Materia
Acceleration of Particles
Cosmic Rays
Interstellar Clouds
Supernova Remnants
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:11336/31804
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/31804
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?Butt, Yousaf M.Torres, Diego F.Combi, Jorge ArielDame, Thomas M.Romero, Gustavo EstebanAcceleration of ParticlesCosmic RaysInterstellar CloudsSupernova Remnantshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The nonthermal supernova remnant (SNR) RX J1713.7-3946 has recently been shown to be a site of cosmic-ray (CR) electron acceleration to TeV energies. Here we present evidence that this remnant is also accelerating CR nuclei. Such energetic nuclei can interact with ambient interstellar gas to produce high-energy gamma rays via the decay of neutral pions. We associate the unidentified EGRET GeV gamma-ray source, 3EG J1714-3857, with a very massive (~3×105 Msolar) and dense (~500 nucleons cm-3) molecular cloud interacting with SNR RX J1713.7-3946. Direct evidence for such interaction is provided by observations of the lowest two rotational transitions of CO molecules in the cloud; as in other clear cases of interaction, the CO(J=2-->1)/CO(J=1-->0) ratio is significantly enhanced. Since the cloud is of low radio and X-ray brightness, electrons cannot be responsible for the bulk of the GeV emission there. A picture thus emerges in which both electrons and nuclei are being accelerated by the SNR: whereas the relativistic electrons dominate the local nonthermal radio, X-ray, and TeV emission, the shock-accelerated CR protons and ions (hadrons) are exposed through their interactions in the adjacent massive cloud, leading to the observed GeV emission via the gamma decay of neutral pions.Fil: Butt, Yousaf M.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Torres, Diego F.. University of Princeton; Estados Unidos. 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. 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: Dame, Thomas M.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Romero, Gustavo Esteban. 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; ArgentinaIOP Publishing2001-12info: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/11336/31804Butt, Yousaf M.; Torres, Diego F.; Combi, Jorge Ariel; Dame, Thomas M.; Romero, Gustavo Esteban; Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?; IOP Publishing; Astrophysical Journal; 562; 2; 12-2001; L167-L1710004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1086/324592info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/324592/metainfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/astro-ph/0109292info:eu-repo/semantics/altIdentifier/url/https://core.ac.uk/reader/159301356info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:20:29Zoai:ri.conicet.gov.ar:11336/31804instacron: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 10:20:29.452CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?
title Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?
spellingShingle Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?
Butt, Yousaf M.
Acceleration of Particles
Cosmic Rays
Interstellar Clouds
Supernova Remnants
title_short Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?
title_full Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?
title_fullStr Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?
title_full_unstemmed Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?
title_sort Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?
dc.creator.none.fl_str_mv Butt, Yousaf M.
Torres, Diego F.
Combi, Jorge Ariel
Dame, Thomas M.
Romero, Gustavo Esteban
author Butt, Yousaf M.
author_facet Butt, Yousaf M.
Torres, Diego F.
Combi, Jorge Ariel
Dame, Thomas M.
Romero, Gustavo Esteban
author_role author
author2 Torres, Diego F.
Combi, Jorge Ariel
Dame, Thomas M.
Romero, Gustavo Esteban
author2_role author
author
author
author
dc.subject.none.fl_str_mv Acceleration of Particles
Cosmic Rays
Interstellar Clouds
Supernova Remnants
topic Acceleration of Particles
Cosmic Rays
Interstellar Clouds
Supernova Remnants
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The nonthermal supernova remnant (SNR) RX J1713.7-3946 has recently been shown to be a site of cosmic-ray (CR) electron acceleration to TeV energies. Here we present evidence that this remnant is also accelerating CR nuclei. Such energetic nuclei can interact with ambient interstellar gas to produce high-energy gamma rays via the decay of neutral pions. We associate the unidentified EGRET GeV gamma-ray source, 3EG J1714-3857, with a very massive (~3×105 Msolar) and dense (~500 nucleons cm-3) molecular cloud interacting with SNR RX J1713.7-3946. Direct evidence for such interaction is provided by observations of the lowest two rotational transitions of CO molecules in the cloud; as in other clear cases of interaction, the CO(J=2-->1)/CO(J=1-->0) ratio is significantly enhanced. Since the cloud is of low radio and X-ray brightness, electrons cannot be responsible for the bulk of the GeV emission there. A picture thus emerges in which both electrons and nuclei are being accelerated by the SNR: whereas the relativistic electrons dominate the local nonthermal radio, X-ray, and TeV emission, the shock-accelerated CR protons and ions (hadrons) are exposed through their interactions in the adjacent massive cloud, leading to the observed GeV emission via the gamma decay of neutral pions.
Fil: Butt, Yousaf M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Torres, Diego F.. University of Princeton; Estados Unidos. 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. 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: Dame, Thomas M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Romero, Gustavo Esteban. 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
description The nonthermal supernova remnant (SNR) RX J1713.7-3946 has recently been shown to be a site of cosmic-ray (CR) electron acceleration to TeV energies. Here we present evidence that this remnant is also accelerating CR nuclei. Such energetic nuclei can interact with ambient interstellar gas to produce high-energy gamma rays via the decay of neutral pions. We associate the unidentified EGRET GeV gamma-ray source, 3EG J1714-3857, with a very massive (~3×105 Msolar) and dense (~500 nucleons cm-3) molecular cloud interacting with SNR RX J1713.7-3946. Direct evidence for such interaction is provided by observations of the lowest two rotational transitions of CO molecules in the cloud; as in other clear cases of interaction, the CO(J=2-->1)/CO(J=1-->0) ratio is significantly enhanced. Since the cloud is of low radio and X-ray brightness, electrons cannot be responsible for the bulk of the GeV emission there. A picture thus emerges in which both electrons and nuclei are being accelerated by the SNR: whereas the relativistic electrons dominate the local nonthermal radio, X-ray, and TeV emission, the shock-accelerated CR protons and ions (hadrons) are exposed through their interactions in the adjacent massive cloud, leading to the observed GeV emission via the gamma decay of neutral pions.
publishDate 2001
dc.date.none.fl_str_mv 2001-12
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/11336/31804
Butt, Yousaf M.; Torres, Diego F.; Combi, Jorge Ariel; Dame, Thomas M.; Romero, Gustavo Esteban; Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?; IOP Publishing; Astrophysical Journal; 562; 2; 12-2001; L167-L171
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/31804
identifier_str_mv Butt, Yousaf M.; Torres, Diego F.; Combi, Jorge Ariel; Dame, Thomas M.; Romero, Gustavo Esteban; Is the supernova remnant RX J1713.7-3946 a hadronic cosmic-ray accelerator?; IOP Publishing; Astrophysical Journal; 562; 2; 12-2001; L167-L171
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1086/324592
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/324592/meta
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/astro-ph/0109292
info:eu-repo/semantics/altIdentifier/url/https://core.ac.uk/reader/159301356
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
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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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