Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures

Autores
Slane, Patrick; Bykov, Andrei; Ellison, Donald C.; Dubner, Gloria Mabel; Castro, Daniel
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and gamma-ray studies have established the presence of relativistic electrons and protons is some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the gamma-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and gamma-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy.
Fil: Slane, Patrick. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Bykov, Andrei. A.F. Ioffe Institute for Physics and Technology; Rusia. St. Petersburg State Polytechnical University; Rusia
Fil: Ellison, Donald C.. University Of North Carolina; Estados Unidos
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: Castro, Daniel. MIT-Kavli Center for Astrophysics and Space Research; Estados Unidos
Materia
Supernova Remnants
Molecular Clouds
X-Rays
Gamma-Rays
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:11336/16498
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signaturesSlane, PatrickBykov, AndreiEllison, Donald C.Dubner, Gloria MabelCastro, DanielSupernova RemnantsMolecular CloudsX-RaysGamma-Rayshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and gamma-ray studies have established the presence of relativistic electrons and protons is some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the gamma-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and gamma-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy.Fil: Slane, Patrick. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Bykov, Andrei. A.F. Ioffe Institute for Physics and Technology; Rusia. St. Petersburg State Polytechnical University; RusiaFil: Ellison, Donald C.. University Of North Carolina; Estados UnidosFil: 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: Castro, Daniel. MIT-Kavli Center for Astrophysics and Space Research; Estados UnidosSpringer2014-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/16498Slane, Patrick; Bykov, Andrei; Ellison, Donald C.; Dubner, Gloria Mabel; Castro, Daniel; Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures; Springer; Space Science Reviews; 188; 1; 7-2014; 1-260038-6308enginfo:eu-repo/semantics/altIdentifier/url/http://link.springer.com/article/10.1007%2Fs11214-014-0062-6info:eu-repo/semantics/altIdentifier/doi/10.1007/s11214-014-0062-6info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:14:49Zoai:ri.conicet.gov.ar:11336/16498instacron: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 10:14:49.843CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures
title Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures
spellingShingle Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures
Slane, Patrick
Supernova Remnants
Molecular Clouds
X-Rays
Gamma-Rays
title_short Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures
title_full Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures
title_fullStr Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures
title_full_unstemmed Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures
title_sort Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures
dc.creator.none.fl_str_mv Slane, Patrick
Bykov, Andrei
Ellison, Donald C.
Dubner, Gloria Mabel
Castro, Daniel
author Slane, Patrick
author_facet Slane, Patrick
Bykov, Andrei
Ellison, Donald C.
Dubner, Gloria Mabel
Castro, Daniel
author_role author
author2 Bykov, Andrei
Ellison, Donald C.
Dubner, Gloria Mabel
Castro, Daniel
author2_role author
author
author
author
dc.subject.none.fl_str_mv Supernova Remnants
Molecular Clouds
X-Rays
Gamma-Rays
topic Supernova Remnants
Molecular Clouds
X-Rays
Gamma-Rays
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 giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and gamma-ray studies have established the presence of relativistic electrons and protons is some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the gamma-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and gamma-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy.
Fil: Slane, Patrick. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Bykov, Andrei. A.F. Ioffe Institute for Physics and Technology; Rusia. St. Petersburg State Polytechnical University; Rusia
Fil: Ellison, Donald C.. University Of North Carolina; Estados Unidos
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: Castro, Daniel. MIT-Kavli Center for Astrophysics and Space Research; Estados Unidos
description The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and gamma-ray studies have established the presence of relativistic electrons and protons is some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the gamma-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and gamma-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy.
publishDate 2014
dc.date.none.fl_str_mv 2014-07
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/11336/16498
Slane, Patrick; Bykov, Andrei; Ellison, Donald C.; Dubner, Gloria Mabel; Castro, Daniel; Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures; Springer; Space Science Reviews; 188; 1; 7-2014; 1-26
0038-6308
url http://hdl.handle.net/11336/16498
identifier_str_mv Slane, Patrick; Bykov, Andrei; Ellison, Donald C.; Dubner, Gloria Mabel; Castro, Daniel; Supernova Remnants interactiong with molecular clouds: X-ray and Gamma-ray signatures; Springer; Space Science Reviews; 188; 1; 7-2014; 1-26
0038-6308
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://link.springer.com/article/10.1007%2Fs11214-014-0062-6
info:eu-repo/semantics/altIdentifier/doi/10.1007/s11214-014-0062-6
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 Springer
publisher.none.fl_str_mv Springer
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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