Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems

Autores
Owocki, S. P.; Romero, Gustavo Esteban; Townsend, R.; Araudo, Anabella Teresa
Año de publicación
2010
Idioma
inglés
Tipo de recurso
documento de conferencia
Estado
versión publicada
Descripción
In the subclass of high-mass X-ray binaries known as “microquasars,” relativistic hadrons in the jets launched by the compact object can interact with cold protons from the stars radiatively driven wind, producing pions that then quickly decay into gamma rays. Since the resulting gamma-ray emissivity depends on the target density, the detection of rapid variability in microquasars with GLAST and the new generation of Cherenkov imaging arrays could be used to probe the clumped structure of the stellar wind. This paper summarizes recent analyses of how the “porosity length” of the stellar wind structure can set the level of fluctuation in gamma rays. A key result is that, for a porosity length defined by h = L/f, i.e. as the ratio of the characteristic size L of clumps to their volume filling factor f, the relative fluctuation in gamma-ray emission in a binary with orbital separation a scales as (h/πa)1/2 in the “thin-jet” limit, and is reduced by a factor 1/sqrt( 1 + phi a/2L ) for a jet with a finite opening angle phi. For a thin jet and quite moderate porosity length h = 0.03a, this implies a ca. 10% variation in the gamma-ray emission.
Fil: Owocki, S. P.. No especifíca;
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
Fil: Townsend, R.. No especifíca;
Fil: Araudo, Anabella Teresa. 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
High Energy Phenomena in Massive Stars
Jaén
España
Universidad de Jaén
Materia
Microquasars
Massive stars: winds
Gamma-rays: theory
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:11336/222320
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Gamma-Ray Variability from Stellar Wind Porosity in Microquasar SystemsOwocki, S. P.Romero, Gustavo EstebanTownsend, R.Araudo, Anabella TeresaMicroquasarsMassive stars: windsGamma-rays: theoryhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1In the subclass of high-mass X-ray binaries known as “microquasars,” relativistic hadrons in the jets launched by the compact object can interact with cold protons from the stars radiatively driven wind, producing pions that then quickly decay into gamma rays. Since the resulting gamma-ray emissivity depends on the target density, the detection of rapid variability in microquasars with GLAST and the new generation of Cherenkov imaging arrays could be used to probe the clumped structure of the stellar wind. This paper summarizes recent analyses of how the “porosity length” of the stellar wind structure can set the level of fluctuation in gamma rays. A key result is that, for a porosity length defined by h = L/f, i.e. as the ratio of the characteristic size L of clumps to their volume filling factor f, the relative fluctuation in gamma-ray emission in a binary with orbital separation a scales as (h/πa)1/2 in the “thin-jet” limit, and is reduced by a factor 1/sqrt( 1 + phi a/2L ) for a jet with a finite opening angle phi. For a thin jet and quite moderate porosity length h = 0.03a, this implies a ca. 10% variation in the gamma-ray emission.Fil: Owocki, S. P.. No especifíca;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; ArgentinaFil: Townsend, R.. No especifíca;Fil: Araudo, Anabella Teresa. 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; ArgentinaHigh Energy Phenomena in Massive StarsJaénEspañaUniversidad de JaénAstronomical Society of the PacificMartí, JosepLuque Escamilla, Pedro L.Combi, Jorge Ariel2010info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectReuniónJournalhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/222320Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems; High Energy Phenomena in Massive Stars; Jaén; España; 2009; 49-549781583817247CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://aspbooks.org/custom/publications/paper/422-0049.htmlinfo:eu-repo/semantics/altIdentifier/url/https://aspbooks.org/a/volumes/table_of_contents/?book_id=437info:eu-repo/semantics/altIdentifier/url/https://articles.adsabs.harvard.edu/full/2010ASPC..422...49OInternacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-10T13:09:29Zoai:ri.conicet.gov.ar:11336/222320instacron: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:34982025-09-10 13:09:29.769CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems
title Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems
spellingShingle Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems
Owocki, S. P.
Microquasars
Massive stars: winds
Gamma-rays: theory
title_short Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems
title_full Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems
title_fullStr Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems
title_full_unstemmed Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems
title_sort Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems
dc.creator.none.fl_str_mv Owocki, S. P.
Romero, Gustavo Esteban
Townsend, R.
Araudo, Anabella Teresa
author Owocki, S. P.
author_facet Owocki, S. P.
Romero, Gustavo Esteban
Townsend, R.
Araudo, Anabella Teresa
author_role author
author2 Romero, Gustavo Esteban
Townsend, R.
Araudo, Anabella Teresa
author2_role author
author
author
dc.contributor.none.fl_str_mv Martí, Josep
Luque Escamilla, Pedro L.
Combi, Jorge Ariel
dc.subject.none.fl_str_mv Microquasars
Massive stars: winds
Gamma-rays: theory
topic Microquasars
Massive stars: winds
Gamma-rays: theory
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv In the subclass of high-mass X-ray binaries known as “microquasars,” relativistic hadrons in the jets launched by the compact object can interact with cold protons from the stars radiatively driven wind, producing pions that then quickly decay into gamma rays. Since the resulting gamma-ray emissivity depends on the target density, the detection of rapid variability in microquasars with GLAST and the new generation of Cherenkov imaging arrays could be used to probe the clumped structure of the stellar wind. This paper summarizes recent analyses of how the “porosity length” of the stellar wind structure can set the level of fluctuation in gamma rays. A key result is that, for a porosity length defined by h = L/f, i.e. as the ratio of the characteristic size L of clumps to their volume filling factor f, the relative fluctuation in gamma-ray emission in a binary with orbital separation a scales as (h/πa)1/2 in the “thin-jet” limit, and is reduced by a factor 1/sqrt( 1 + phi a/2L ) for a jet with a finite opening angle phi. For a thin jet and quite moderate porosity length h = 0.03a, this implies a ca. 10% variation in the gamma-ray emission.
Fil: Owocki, S. P.. No especifíca;
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
Fil: Townsend, R.. No especifíca;
Fil: Araudo, Anabella Teresa. 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
High Energy Phenomena in Massive Stars
Jaén
España
Universidad de Jaén
description In the subclass of high-mass X-ray binaries known as “microquasars,” relativistic hadrons in the jets launched by the compact object can interact with cold protons from the stars radiatively driven wind, producing pions that then quickly decay into gamma rays. Since the resulting gamma-ray emissivity depends on the target density, the detection of rapid variability in microquasars with GLAST and the new generation of Cherenkov imaging arrays could be used to probe the clumped structure of the stellar wind. This paper summarizes recent analyses of how the “porosity length” of the stellar wind structure can set the level of fluctuation in gamma rays. A key result is that, for a porosity length defined by h = L/f, i.e. as the ratio of the characteristic size L of clumps to their volume filling factor f, the relative fluctuation in gamma-ray emission in a binary with orbital separation a scales as (h/πa)1/2 in the “thin-jet” limit, and is reduced by a factor 1/sqrt( 1 + phi a/2L ) for a jet with a finite opening angle phi. For a thin jet and quite moderate porosity length h = 0.03a, this implies a ca. 10% variation in the gamma-ray emission.
publishDate 2010
dc.date.none.fl_str_mv 2010
dc.type.none.fl_str_mv info:eu-repo/semantics/publishedVersion
info:eu-repo/semantics/conferenceObject
Reunión
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/11336/222320
Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems; High Energy Phenomena in Massive Stars; Jaén; España; 2009; 49-54
9781583817247
CONICET Digital
CONICET
url http://hdl.handle.net/11336/222320
identifier_str_mv Gamma-Ray Variability from Stellar Wind Porosity in Microquasar Systems; High Energy Phenomena in Massive Stars; Jaén; España; 2009; 49-54
9781583817247
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://aspbooks.org/custom/publications/paper/422-0049.html
info:eu-repo/semantics/altIdentifier/url/https://aspbooks.org/a/volumes/table_of_contents/?book_id=437
info:eu-repo/semantics/altIdentifier/url/https://articles.adsabs.harvard.edu/full/2010ASPC..422...49O
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.coverage.none.fl_str_mv Internacional
dc.publisher.none.fl_str_mv Astronomical Society of the Pacific
publisher.none.fl_str_mv Astronomical Society of the Pacific
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 12.993085

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