Using gamma-rays to probe the clumped structure of stellar winds
- Autores
- Romero, Gustavo Esteban; Owocki, S. P.; Araudo, Anabella Teresa; Townsend, R. H. D.; Benaglia, Paula
- Año de publicación
- 2009
- Idioma
- inglés
- Tipo de recurso
- documento de conferencia
- Estado
- versión publicada
- Descripción
- Gamma-rays can be produced by the interaction of a relativistic jet and the matter of the stellar wind in the subclass of massive X-ray binaries known as “microquasars”. The relativistic jet is ejected from the surroundings of the compact object and interacts with cold protons from the stellar 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. In particular, we show here that the relative fluctuation in gamma rays may scale with the square root of the ratio of porosity length to binary separation, p h/a, implying for example a ca. 10% variation in gamma ray emission for a quite moderate porosity, h/a ∼ 0.01
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: Owocki, S. P.. University of Delaware; Estados Unidos
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
Fil: Townsend, R. H. D.. University of Delaware; Estados Unidos
Fil: Benaglia, Paula. 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
Clumping in hot-star winds
Postdam
Alemania
Universidad de Postdam - Materia
- stellar winds
- Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/228615
Ver los metadatos del registro completo
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Using gamma-rays to probe the clumped structure of stellar windsRomero, Gustavo EstebanOwocki, S. P.Araudo, Anabella TeresaTownsend, R. H. D.Benaglia, Paulastellar windshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Gamma-rays can be produced by the interaction of a relativistic jet and the matter of the stellar wind in the subclass of massive X-ray binaries known as “microquasars”. The relativistic jet is ejected from the surroundings of the compact object and interacts with cold protons from the stellar 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. In particular, we show here that the relative fluctuation in gamma rays may scale with the square root of the ratio of porosity length to binary separation, p h/a, implying for example a ca. 10% variation in gamma ray emission for a quite moderate porosity, h/a ∼ 0.01Fil: 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: Owocki, S. P.. University of Delaware; Estados UnidosFil: 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; ArgentinaFil: Townsend, R. H. D.. University of Delaware; Estados UnidosFil: Benaglia, Paula. 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; ArgentinaClumping in hot-star windsPostdamAlemaniaUniversidad de PostdamPostdam UniversityHamann, W. -R.Feldmeier, A.Oskinova, L.2009info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectWorkshopBookhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/228615Using gamma-rays to probe the clumped structure of stellar winds; Clumping in hot-star winds; Postdam; Alemania; 2007; 191-194978-3-940793-33-1CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://publishup.uni-potsdam.de/frontdoor/index/index/docId/1574info:eu-repo/semantics/altIdentifier/url/https://ui.adsabs.harvard.edu/abs/2008cihw.conf..191R/abstractInternacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:39:16Zoai:ri.conicet.gov.ar:11336/228615instacron: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 11:39:16.359CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Using gamma-rays to probe the clumped structure of stellar winds |
| title |
Using gamma-rays to probe the clumped structure of stellar winds |
| spellingShingle |
Using gamma-rays to probe the clumped structure of stellar winds Romero, Gustavo Esteban stellar winds |
| title_short |
Using gamma-rays to probe the clumped structure of stellar winds |
| title_full |
Using gamma-rays to probe the clumped structure of stellar winds |
| title_fullStr |
Using gamma-rays to probe the clumped structure of stellar winds |
| title_full_unstemmed |
Using gamma-rays to probe the clumped structure of stellar winds |
| title_sort |
Using gamma-rays to probe the clumped structure of stellar winds |
| dc.creator.none.fl_str_mv |
Romero, Gustavo Esteban Owocki, S. P. Araudo, Anabella Teresa Townsend, R. H. D. Benaglia, Paula |
| author |
Romero, Gustavo Esteban |
| author_facet |
Romero, Gustavo Esteban Owocki, S. P. Araudo, Anabella Teresa Townsend, R. H. D. Benaglia, Paula |
| author_role |
author |
| author2 |
Owocki, S. P. Araudo, Anabella Teresa Townsend, R. H. D. Benaglia, Paula |
| author2_role |
author author author author |
| dc.contributor.none.fl_str_mv |
Hamann, W. -R. Feldmeier, A. Oskinova, L. |
| dc.subject.none.fl_str_mv |
stellar winds |
| topic |
stellar winds |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
Gamma-rays can be produced by the interaction of a relativistic jet and the matter of the stellar wind in the subclass of massive X-ray binaries known as “microquasars”. The relativistic jet is ejected from the surroundings of the compact object and interacts with cold protons from the stellar 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. In particular, we show here that the relative fluctuation in gamma rays may scale with the square root of the ratio of porosity length to binary separation, p h/a, implying for example a ca. 10% variation in gamma ray emission for a quite moderate porosity, h/a ∼ 0.01 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: Owocki, S. P.. University of Delaware; Estados Unidos 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 Fil: Townsend, R. H. D.. University of Delaware; Estados Unidos Fil: Benaglia, Paula. 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 Clumping in hot-star winds Postdam Alemania Universidad de Postdam |
| description |
Gamma-rays can be produced by the interaction of a relativistic jet and the matter of the stellar wind in the subclass of massive X-ray binaries known as “microquasars”. The relativistic jet is ejected from the surroundings of the compact object and interacts with cold protons from the stellar 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. In particular, we show here that the relative fluctuation in gamma rays may scale with the square root of the ratio of porosity length to binary separation, p h/a, implying for example a ca. 10% variation in gamma ray emission for a quite moderate porosity, h/a ∼ 0.01 |
| 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 Workshop Book http://purl.org/coar/resource_type/c_5794 info:ar-repo/semantics/documentoDeConferencia |
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publishedVersion |
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conferenceObject |
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http://hdl.handle.net/11336/228615 Using gamma-rays to probe the clumped structure of stellar winds; Clumping in hot-star winds; Postdam; Alemania; 2007; 191-194 978-3-940793-33-1 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/228615 |
| identifier_str_mv |
Using gamma-rays to probe the clumped structure of stellar winds; Clumping in hot-star winds; Postdam; Alemania; 2007; 191-194 978-3-940793-33-1 CONICET Digital CONICET |
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eng |
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eng |
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Internacional |
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Postdam University |
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Postdam University |
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