The proton microquasar

Autores
Vila, Gabriela Soledad; Romero, Gustavo Esteban
Año de publicación
2009
Idioma
inglés
Tipo de recurso
documento de conferencia
Estado
versión publicada
Descripción
We present a model for high-energy emission in microquasars where the energy content of the jets is dominated by relativistic protons. We also include a primary leptonic component. Particles are accelerated up to relativistic energies in a compact region located near the base of the jet, where most of the emission is produced. We calculate the production spectrum due to proton and electron synchrotron radiation and photohadronic interactions. The target field for proton-photon collisions is provided by the synchrotron radiation in the acceleration region. In models with a significant leptonic component, strong internal photon-photon absorption can attenuate the emission spectrum at high energies.Depending on the values of the parameters, our model predicts luminosities in the range 10^34  - 10^37 erg/s up to GeV energies, with a high-energy tail that can extend up to 10^16 eV. In some cases, however, absorption effects can completely suppress the emission above 10 GeV, giving rise to different spectral shapes. These results can be tested in the near future by observations with instruments like GLAST-Fermi, HESS II and MAGIC II.
Fil: Vila, Gabriela Soledad. 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: Romero, Gustavo Esteban. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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
Fourth Heidelberg International Symposium on High Energy Gamma-Ray Astronomy
Heidelberg
Alemania
Max-Planck-Institute for Nuclear Physics
Materia
X-ray binaries
Gamma-ray sources
Gamma-ray
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:11336/228086
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/228086
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The proton microquasarVila, Gabriela SoledadRomero, Gustavo EstebanX-ray binariesGamma-ray sourcesGamma-rayhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present a model for high-energy emission in microquasars where the energy content of the jets is dominated by relativistic protons. We also include a primary leptonic component. Particles are accelerated up to relativistic energies in a compact region located near the base of the jet, where most of the emission is produced. We calculate the production spectrum due to proton and electron synchrotron radiation and photohadronic interactions. The target field for proton-photon collisions is provided by the synchrotron radiation in the acceleration region. In models with a significant leptonic component, strong internal photon-photon absorption can attenuate the emission spectrum at high energies.Depending on the values of the parameters, our model predicts luminosities in the range 10^34  - 10^37 erg/s up to GeV energies, with a high-energy tail that can extend up to 10^16 eV. In some cases, however, absorption effects can completely suppress the emission above 10 GeV, giving rise to different spectral shapes. These results can be tested in the near future by observations with instruments like GLAST-Fermi, HESS II and MAGIC II.Fil: Vila, Gabriela Soledad. 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: Romero, Gustavo Esteban. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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; ArgentinaFourth Heidelberg International Symposium on High Energy Gamma-Ray AstronomyHeidelbergAlemaniaMax-Planck-Institute for Nuclear PhysicsAmerican Institute of PhysicsAharonian, Felix A.Hofmann, WernerRieger, Frank2009info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectSimposioJournalhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/228086The proton microquasar; Fourth Heidelberg International Symposium on High Energy Gamma-Ray Astronomy; Heidelberg; Alemania; 2008; 289-29297807354061620094-243XCONICET DigitalCONICETenghttps://inspirehep.net/literature/1391412info:eu-repo/semantics/altIdentifier/url/https://ui.adsabs.harvard.edu/abs/2008AIPC.1085..289V/abstractinfo:eu-repo/semantics/altIdentifier/doi/10.1063/1.3076662Internacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:46:59Zoai:ri.conicet.gov.ar:11336/228086instacron: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 10:47:00.035CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The proton microquasar
title The proton microquasar
spellingShingle The proton microquasar
Vila, Gabriela Soledad
X-ray binaries
Gamma-ray sources
Gamma-ray
title_short The proton microquasar
title_full The proton microquasar
title_fullStr The proton microquasar
title_full_unstemmed The proton microquasar
title_sort The proton microquasar
dc.creator.none.fl_str_mv Vila, Gabriela Soledad
Romero, Gustavo Esteban
author Vila, Gabriela Soledad
author_facet Vila, Gabriela Soledad
Romero, Gustavo Esteban
author_role author
author2 Romero, Gustavo Esteban
author2_role author
dc.contributor.none.fl_str_mv Aharonian, Felix A.
Hofmann, Werner
Rieger, Frank
dc.subject.none.fl_str_mv X-ray binaries
Gamma-ray sources
Gamma-ray
topic X-ray binaries
Gamma-ray sources
Gamma-ray
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present a model for high-energy emission in microquasars where the energy content of the jets is dominated by relativistic protons. We also include a primary leptonic component. Particles are accelerated up to relativistic energies in a compact region located near the base of the jet, where most of the emission is produced. We calculate the production spectrum due to proton and electron synchrotron radiation and photohadronic interactions. The target field for proton-photon collisions is provided by the synchrotron radiation in the acceleration region. In models with a significant leptonic component, strong internal photon-photon absorption can attenuate the emission spectrum at high energies.Depending on the values of the parameters, our model predicts luminosities in the range 10^34  - 10^37 erg/s up to GeV energies, with a high-energy tail that can extend up to 10^16 eV. In some cases, however, absorption effects can completely suppress the emission above 10 GeV, giving rise to different spectral shapes. These results can be tested in the near future by observations with instruments like GLAST-Fermi, HESS II and MAGIC II.
Fil: Vila, Gabriela Soledad. 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: Romero, Gustavo Esteban. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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
Fourth Heidelberg International Symposium on High Energy Gamma-Ray Astronomy
Heidelberg
Alemania
Max-Planck-Institute for Nuclear Physics
description We present a model for high-energy emission in microquasars where the energy content of the jets is dominated by relativistic protons. We also include a primary leptonic component. Particles are accelerated up to relativistic energies in a compact region located near the base of the jet, where most of the emission is produced. We calculate the production spectrum due to proton and electron synchrotron radiation and photohadronic interactions. The target field for proton-photon collisions is provided by the synchrotron radiation in the acceleration region. In models with a significant leptonic component, strong internal photon-photon absorption can attenuate the emission spectrum at high energies.Depending on the values of the parameters, our model predicts luminosities in the range 10^34  - 10^37 erg/s up to GeV energies, with a high-energy tail that can extend up to 10^16 eV. In some cases, however, absorption effects can completely suppress the emission above 10 GeV, giving rise to different spectral shapes. These results can be tested in the near future by observations with instruments like GLAST-Fermi, HESS II and MAGIC II.
publishDate 2009
dc.date.none.fl_str_mv 2009
dc.type.none.fl_str_mv info:eu-repo/semantics/publishedVersion
info:eu-repo/semantics/conferenceObject
Simposio
Journal
http://purl.org/coar/resource_type/c_5794
info:ar-repo/semantics/documentoDeConferencia
status_str publishedVersion
format conferenceObject
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/228086
The proton microquasar; Fourth Heidelberg International Symposium on High Energy Gamma-Ray Astronomy; Heidelberg; Alemania; 2008; 289-292
9780735406162
0094-243X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/228086
identifier_str_mv The proton microquasar; Fourth Heidelberg International Symposium on High Energy Gamma-Ray Astronomy; Heidelberg; Alemania; 2008; 289-292
9780735406162
0094-243X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv https://inspirehep.net/literature/1391412
info:eu-repo/semantics/altIdentifier/url/https://ui.adsabs.harvard.edu/abs/2008AIPC.1085..289V/abstract
info:eu-repo/semantics/altIdentifier/doi/10.1063/1.3076662
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.coverage.none.fl_str_mv Internacional
dc.publisher.none.fl_str_mv American Institute of Physics
publisher.none.fl_str_mv American Institute of Physics
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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