Very high-energy gamma-ray emission from X-ray transients during major outbursts
- Autores
- Orellana, Mariana Dominga; Romero, Gustavo E.; Pellizza González, Leonardo J.; Vidrih, S.
- Año de publicación
- 2007
- Idioma
- español castellano
- Tipo de recurso
- artículo
- Estado
- versión aceptada
- Descripción
- Fil: Orellana, Mariana D. Comision de Investigaciones Científicas; Argentina
Fil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Orellana, Mariana D. Universidad Nacional de Río Negro; Argentina
Fil: Orellana, Mariana D. Instituto Argentino de Radioastronomia; Argentina
Fil: Romero, Gustavo E. Comisión de Investigaciones Científicas; Argentina
Fil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; Argentina
Fil: Pellizza González, Leonardo J. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria; Argentina
Fil: Pellizza González, Leonardo J. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales.
Fil: Pellizza González, Leonardo J. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Vidrih, S. University of Cambridge; Reino Unido
Some high mass X-ray binaries (HMXB) have been recently confirmed as γ-ray sources by ground based Cherenkov telescopes. In this work, we discuss the γ-ray emission from X-ray transient sources formed by a Be star and a highly magnetized neutron star. This kind of systems can produce variable hadronic γ-ray emission through the mechanism proposed by Cheng and Ruderman, where a proton beam accelerated in the pulsar magnetosphere impacts the transient accretion disk. We choose as case of study the best known system of this class: A0535+26. Aims. We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. Methods. We study the gamma-ray emission generated during a major X-ray outburst of a HMXB adopting for the model the parameters of A0535+26. The emerging photon signal from the disk is determined by the grammage of the disk that modulates the optical depth. The electromagnetic cascades initiated by photons absorbed in the disk are explored, making use of the so-called “Approximation A” to solve the cascade equations. Very high energy photons induce Inverse Compton cascades in the photon field of the massive star. We implemented Monte Carlo simulations of these cascades, in order to estimate the characteristics of the resulting spectrum. Results. TeV emission should be detectable by Cherenkov telescopes during a major X-ray outburst of a binary formed by a Be star and a highly magnetized neutron star. The γ-ray light curve is found to evolve in anti-correlation with the X-ray signal. - Materia
-
Astronomía
X-ray: Binaries
Gamma-Rays: Theory
Stars: Individual: A0535+26
Astronomía - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de Río Negro
- OAI Identificador
- oai:rid.unrn.edu.ar:20.500.12049/2835
Ver los metadatos del registro completo
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Very high-energy gamma-ray emission from X-ray transients during major outburstsOrellana, Mariana DomingaRomero, Gustavo E.Pellizza González, Leonardo J.Vidrih, S.AstronomíaX-ray: BinariesGamma-Rays: TheoryStars: Individual: A0535+26AstronomíaFil: Orellana, Mariana D. Comision de Investigaciones Científicas; ArgentinaFil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; ArgentinaFil: Orellana, Mariana D. Universidad Nacional de Río Negro; ArgentinaFil: Orellana, Mariana D. Instituto Argentino de Radioastronomia; ArgentinaFil: Romero, Gustavo E. Comisión de Investigaciones Científicas; ArgentinaFil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; ArgentinaFil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; ArgentinaFil: Pellizza González, Leonardo J. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria; ArgentinaFil: Pellizza González, Leonardo J. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales.Fil: Pellizza González, Leonardo J. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Vidrih, S. University of Cambridge; Reino UnidoSome high mass X-ray binaries (HMXB) have been recently confirmed as γ-ray sources by ground based Cherenkov telescopes. In this work, we discuss the γ-ray emission from X-ray transient sources formed by a Be star and a highly magnetized neutron star. This kind of systems can produce variable hadronic γ-ray emission through the mechanism proposed by Cheng and Ruderman, where a proton beam accelerated in the pulsar magnetosphere impacts the transient accretion disk. We choose as case of study the best known system of this class: A0535+26. Aims. We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. Methods. We study the gamma-ray emission generated during a major X-ray outburst of a HMXB adopting for the model the parameters of A0535+26. The emerging photon signal from the disk is determined by the grammage of the disk that modulates the optical depth. The electromagnetic cascades initiated by photons absorbed in the disk are explored, making use of the so-called “Approximation A” to solve the cascade equations. Very high energy photons induce Inverse Compton cascades in the photon field of the massive star. We implemented Monte Carlo simulations of these cascades, in order to estimate the characteristics of the resulting spectrum. Results. TeV emission should be detectable by Cherenkov telescopes during a major X-ray outburst of a binary formed by a Be star and a highly magnetized neutron star. The γ-ray light curve is found to evolve in anti-correlation with the X-ray signal.EDP Sciences2007-01-14info:eu-repo/semantics/articleinfo:eu-repo/semantics/acceptedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfOrellana, Mariana D., Romero, Gustavo E., Pellizza González, Leonardo J. & Vidrih, S. (2007). Very high-energy gamma-ray emission from X-ray transients during major outbursts. EDP Sciences; Astronomy and Astrophysics; 465; 3; 703-7090004-63611432-0746https://www.aanda.org/articles/aa/abs/2007/15/aa6238-06/aa6238-06.htmlhttps://arxiv.org/abs/astro-ph/0701695http://hdl.handle.net/11336/21951https://rid.unrn.edu.ar/jspui/handle/20.500.12049/2835http://dx.doi.org/10.1051/0004-6361:20066238spa465Astronomy and Astrophysicsinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/4.0/reponame:RID-UNRN (UNRN)instname:Universidad Nacional de Río Negro2025-09-04T11:12:47Zoai:rid.unrn.edu.ar:20.500.12049/2835instacron:UNRNInstitucionalhttps://rid.unrn.edu.ar/jspui/Universidad públicaNo correspondehttps://rid.unrn.edu.ar/oai/snrdrid@unrn.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:43692025-09-04 11:12:47.691RID-UNRN (UNRN) - Universidad Nacional de Río Negrofalse |
| dc.title.none.fl_str_mv |
Very high-energy gamma-ray emission from X-ray transients during major outbursts |
| title |
Very high-energy gamma-ray emission from X-ray transients during major outbursts |
| spellingShingle |
Very high-energy gamma-ray emission from X-ray transients during major outbursts Orellana, Mariana Dominga Astronomía X-ray: Binaries Gamma-Rays: Theory Stars: Individual: A0535+26 Astronomía |
| title_short |
Very high-energy gamma-ray emission from X-ray transients during major outbursts |
| title_full |
Very high-energy gamma-ray emission from X-ray transients during major outbursts |
| title_fullStr |
Very high-energy gamma-ray emission from X-ray transients during major outbursts |
| title_full_unstemmed |
Very high-energy gamma-ray emission from X-ray transients during major outbursts |
| title_sort |
Very high-energy gamma-ray emission from X-ray transients during major outbursts |
| dc.creator.none.fl_str_mv |
Orellana, Mariana Dominga Romero, Gustavo E. Pellizza González, Leonardo J. Vidrih, S. |
| author |
Orellana, Mariana Dominga |
| author_facet |
Orellana, Mariana Dominga Romero, Gustavo E. Pellizza González, Leonardo J. Vidrih, S. |
| author_role |
author |
| author2 |
Romero, Gustavo E. Pellizza González, Leonardo J. Vidrih, S. |
| author2_role |
author author author |
| dc.subject.none.fl_str_mv |
Astronomía X-ray: Binaries Gamma-Rays: Theory Stars: Individual: A0535+26 Astronomía |
| topic |
Astronomía X-ray: Binaries Gamma-Rays: Theory Stars: Individual: A0535+26 Astronomía |
| dc.description.none.fl_txt_mv |
Fil: Orellana, Mariana D. Comision de Investigaciones Científicas; Argentina Fil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina Fil: Orellana, Mariana D. Universidad Nacional de Río Negro; Argentina Fil: Orellana, Mariana D. Instituto Argentino de Radioastronomia; Argentina Fil: Romero, Gustavo E. Comisión de Investigaciones Científicas; Argentina Fil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina Fil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; Argentina Fil: Pellizza González, Leonardo J. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria; Argentina Fil: Pellizza González, Leonardo J. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Fil: Pellizza González, Leonardo J. Instituto de Astronomía y Física del Espacio; Argentina Fil: Vidrih, S. University of Cambridge; Reino Unido Some high mass X-ray binaries (HMXB) have been recently confirmed as γ-ray sources by ground based Cherenkov telescopes. In this work, we discuss the γ-ray emission from X-ray transient sources formed by a Be star and a highly magnetized neutron star. This kind of systems can produce variable hadronic γ-ray emission through the mechanism proposed by Cheng and Ruderman, where a proton beam accelerated in the pulsar magnetosphere impacts the transient accretion disk. We choose as case of study the best known system of this class: A0535+26. Aims. We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. Methods. We study the gamma-ray emission generated during a major X-ray outburst of a HMXB adopting for the model the parameters of A0535+26. The emerging photon signal from the disk is determined by the grammage of the disk that modulates the optical depth. The electromagnetic cascades initiated by photons absorbed in the disk are explored, making use of the so-called “Approximation A” to solve the cascade equations. Very high energy photons induce Inverse Compton cascades in the photon field of the massive star. We implemented Monte Carlo simulations of these cascades, in order to estimate the characteristics of the resulting spectrum. Results. TeV emission should be detectable by Cherenkov telescopes during a major X-ray outburst of a binary formed by a Be star and a highly magnetized neutron star. The γ-ray light curve is found to evolve in anti-correlation with the X-ray signal. |
| description |
Fil: Orellana, Mariana D. Comision de Investigaciones Científicas; Argentina |
| publishDate |
2007 |
| dc.date.none.fl_str_mv |
2007-01-14 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/acceptedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
| format |
article |
| status_str |
acceptedVersion |
| dc.identifier.none.fl_str_mv |
Orellana, Mariana D., Romero, Gustavo E., Pellizza González, Leonardo J. & Vidrih, S. (2007). Very high-energy gamma-ray emission from X-ray transients during major outbursts. EDP Sciences; Astronomy and Astrophysics; 465; 3; 703-709 0004-6361 1432-0746 https://www.aanda.org/articles/aa/abs/2007/15/aa6238-06/aa6238-06.html https://arxiv.org/abs/astro-ph/0701695 http://hdl.handle.net/11336/21951 https://rid.unrn.edu.ar/jspui/handle/20.500.12049/2835 http://dx.doi.org/10.1051/0004-6361:20066238 |
| identifier_str_mv |
Orellana, Mariana D., Romero, Gustavo E., Pellizza González, Leonardo J. & Vidrih, S. (2007). Very high-energy gamma-ray emission from X-ray transients during major outbursts. EDP Sciences; Astronomy and Astrophysics; 465; 3; 703-709 0004-6361 1432-0746 |
| url |
https://www.aanda.org/articles/aa/abs/2007/15/aa6238-06/aa6238-06.html https://arxiv.org/abs/astro-ph/0701695 http://hdl.handle.net/11336/21951 https://rid.unrn.edu.ar/jspui/handle/20.500.12049/2835 http://dx.doi.org/10.1051/0004-6361:20066238 |
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spa |
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spa |
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465 Astronomy and Astrophysics |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/4.0/ |
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openAccess |
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EDP Sciences |
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EDP Sciences |
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