Very high energy γ-ray emission from X-ray transients during major outbursts
- Autores
- Orellana, Mariana Dominga; Romero, Gustavo Esteban; Pellizza, L. J.; Vidrih, S.
- Año de publicación
- 2007
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. 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 y-ray light curve is found to evolve in anti-correlation with the X-ray signal.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Gamma-rays: theory
Stars: individual: A0535+26
X-ray: binaries - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/83002
Ver los metadatos del registro completo
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Very high energy γ-ray emission from X-ray transients during major outburstsOrellana, Mariana DomingaRomero, Gustavo EstebanPellizza, L. J.Vidrih, S.Ciencias AstronómicasGamma-rays: theoryStars: individual: A0535+26X-ray: binaries<b>Context.</b> 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. <b>Aims.</b> We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. <b>Methods.</b> 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. <b>Results.</b> 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 y-ray light curve is found to evolve in anti-correlation with the X-ray signal.Facultad de Ciencias Astronómicas y Geofísicas2007-01-22info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf703-709http://sedici.unlp.edu.ar/handle/10915/83002enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066238info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-03T10:48:00Zoai:sedici.unlp.edu.ar:10915/83002Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-03 10:48:01.026SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
Very high energy γ-ray emission from X-ray transients during major outbursts |
| title |
Very high energy γ-ray emission from X-ray transients during major outbursts |
| spellingShingle |
Very high energy γ-ray emission from X-ray transients during major outbursts Orellana, Mariana Dominga Ciencias Astronómicas Gamma-rays: theory Stars: individual: A0535+26 X-ray: binaries |
| title_short |
Very high energy γ-ray emission from X-ray transients during major outbursts |
| title_full |
Very high energy γ-ray emission from X-ray transients during major outbursts |
| title_fullStr |
Very high energy γ-ray emission from X-ray transients during major outbursts |
| title_full_unstemmed |
Very high energy γ-ray emission from X-ray transients during major outbursts |
| title_sort |
Very high energy γ-ray emission from X-ray transients during major outbursts |
| dc.creator.none.fl_str_mv |
Orellana, Mariana Dominga Romero, Gustavo Esteban Pellizza, L. J. Vidrih, S. |
| author |
Orellana, Mariana Dominga |
| author_facet |
Orellana, Mariana Dominga Romero, Gustavo Esteban Pellizza, L. J. Vidrih, S. |
| author_role |
author |
| author2 |
Romero, Gustavo Esteban Pellizza, L. J. Vidrih, S. |
| author2_role |
author author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas Gamma-rays: theory Stars: individual: A0535+26 X-ray: binaries |
| topic |
Ciencias Astronómicas Gamma-rays: theory Stars: individual: A0535+26 X-ray: binaries |
| dc.description.none.fl_txt_mv |
<b>Context.</b> 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. <b>Aims.</b> We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. <b>Methods.</b> 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. <b>Results.</b> 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 y-ray light curve is found to evolve in anti-correlation with the X-ray signal. Facultad de Ciencias Astronómicas y Geofísicas |
| description |
<b>Context.</b> 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. <b>Aims.</b> We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. <b>Methods.</b> 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. <b>Results.</b> 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 y-ray light curve is found to evolve in anti-correlation with the X-ray signal. |
| publishDate |
2007 |
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2007-01-22 |
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