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dc.contributor.author
Romero, Gustavo Esteban
dc.contributor.author
Okazaki, A. T.
dc.contributor.author
Orellana, Mariana Dominga
dc.contributor.author
Owocki, S. P.
dc.date.available
2017-11-30T17:12:40Z
dc.date.issued
2007-12
dc.identifier.citation
Romero, Gustavo Esteban; Okazaki, A. T.; Orellana, Mariana Dominga; Owocki, S. P.; Accretion vs. colliding wind models for the gamma-ray binary LS I +61 303: an assessment; EDP Sciences; Astronomy and Astrophysics; 474; 1; 12-2007; 15-22
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/29336
dc.description.abstract
Context. LS I +61 303 is a puzzling Be/X-ray binary with variable gamma-ray emission up to TeV energies. The nature of the compact object and the origin of the high-energy emission are unclear. One family of models invokes particle acceleration in shocks from the collision between the B-star wind and a relativistic pulsar wind, whereas another centers on a relativistic jet powered by accretion from the Be star decretion disc onto a black hole. Recent high-resolution radio observations showing a putative “cometary tail” pointing away from the Be star near periastron have been cited as support for the pulsar-wind model. Aims. We wish to carry out a quantitative assessment of these competing models. Methods. We apply a “Smoothed Particle Hydrodynamics” (SPH) code in 3D dynamical simulations for both the pulsar-windinteraction and accretion-jet models. The former yields a dynamical description of the shape of the wind-wind interaction surface. The latter provides a dynamical estimation of the accretion rate under a variety of conditions, and how this varies with orbital phase. Results. The results allow critical evaluation of how the two distinct models confront the data in various wavebands. When one accounts for the 3D dynamical wind interaction under realistic constraints for the relative strength of the B-star and pulsar winds, the resulting form of the interaction front does not match the putative “cometary tail” claimed from radio observations. On the other hand, dynamical simulations of the accretion-jet model indicate that the orbital phase variation of accretion power includes a secondary broad peak well away from periastron, thus providing a plausible way to explain the observed TeV gamma ray emission toward apastron. Conclusions. Contrary to previous claims, the colliding-wind model is not clearly established for LS I +61 303, whereas the accretionjet model can reproduce many key characteristics, such as required energy budget, lightcurve, and spectrum of the observed TeV gamma-ray emission.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
X Ray Binaries
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Gamma Rays
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Ls I +61 303 (Estrella)
dc.subject.classification
Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
Accretion vs. colliding wind models for the gamma-ray binary LS I +61 303: an assessment
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2017-10-12T19:38:06Z
dc.journal.volume
474
dc.journal.number
1
dc.journal.pagination
15-22
dc.journal.pais
Francia
dc.journal.ciudad
Les Ulis Cedex A
dc.description.fil
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
dc.description.fil
Fil: Okazaki, A. T.. Hokkai-Gaukuen University; Japón
dc.description.fil
Fil: Orellana, Mariana Dominga. 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
dc.description.fil
Fil: Owocki, S. P.. University of Delaware; Estados Unidos
dc.journal.title
Astronomy and Astrophysics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361:20078035


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