The major role of eccentricity in the evolution of colliding pulsar-stellar winds

Binary systems that host a massive star and a non-accreting pulsar can be powerful non-thermal emitters. The relativistic pulsar wind and the non-relativistic stellar outflows interact along the orbit, producing ultrarelativistic particles that radiate from radio to gamma rays. To properly character...

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Detalles Bibliográficos
Autores: Barkov, M., Bosch-Ramon, Valentí
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2021
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/262258
Acceso en línea:http://hdl.handle.net/10261/262258
Access Level:acceso abierto
Palabra clave:Hydrodynamics
Stars: winds
Outflows
Gamma-rays: stars
X-ray binaries
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spelling The major role of eccentricity in the evolution of colliding pulsar-stellar windsBarkov, M.Bosch-Ramon, ValentíHydrodynamicsStars: windsOutflowsGamma-rays: starsX-ray binariesBinary systems that host a massive star and a non-accreting pulsar can be powerful non-thermal emitters. The relativistic pulsar wind and the non-relativistic stellar outflows interact along the orbit, producing ultrarelativistic particles that radiate from radio to gamma rays. To properly characterize the physics of these sources, and better understand their emission and impact on the environment, careful modeling of the outflow interactions, spanning a broad range of spatial and temporal scales, is needed. Full three-dimensional approaches are very computationally expensive, but simpler approximate approaches, while still realistic at the semi-quantitative level, are available. We present here the results of calculations done with a quasi three-dimensional scheme to compute the evolution of the interacting flows in a region spanning in size up to a thousand times the size of the binary. In particular, we analyze for the first time the role of different eccentricities in the large scale evolution of the shocked flows. We find that the higher the eccentricity, the closer the flows behave like a one-side outflow, which becomes rather collimated for eccentricity values >0.75. The simulations also unveil that the pulsar and the stellar winds become fully mixed within the grid for low eccentricity systems, presenting a more stochastic behavior at large scales than in the highly eccentric systems.V.B.-R. acknowledges financial support by the State Agency for Research of the Spanish Ministry of Science and Innovation under grant PID2019-105510GB-C31 and through the ”Unit of Excellence María de Maeztu 2020-2023” award to the Institute of Cosmos Sciences (CEX2019-000918- M), and by the Catalan DEC grant 2017 SGR 643.Multidisciplinary Digital Publishing InstituteMinisterio de Ciencia, Innovación y Universidades (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2022202220212022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/262258reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-105510GB-C31http://doi.org/10.3390/universe7080277Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2622582026-05-22T06:33:51Z
dc.title.none.fl_str_mv The major role of eccentricity in the evolution of colliding pulsar-stellar winds
title The major role of eccentricity in the evolution of colliding pulsar-stellar winds
spellingShingle The major role of eccentricity in the evolution of colliding pulsar-stellar winds
Barkov, M.
Hydrodynamics
Stars: winds
Outflows
Gamma-rays: stars
X-ray binaries
title_short The major role of eccentricity in the evolution of colliding pulsar-stellar winds
title_full The major role of eccentricity in the evolution of colliding pulsar-stellar winds
title_fullStr The major role of eccentricity in the evolution of colliding pulsar-stellar winds
title_full_unstemmed The major role of eccentricity in the evolution of colliding pulsar-stellar winds
title_sort The major role of eccentricity in the evolution of colliding pulsar-stellar winds
dc.creator.none.fl_str_mv Barkov, M.
Bosch-Ramon, Valentí
author Barkov, M.
author_facet Barkov, M.
Bosch-Ramon, Valentí
author_role author
author2 Bosch-Ramon, Valentí
author2_role author
dc.contributor.none.fl_str_mv Ministerio de Ciencia, Innovación y Universidades (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Hydrodynamics
Stars: winds
Outflows
Gamma-rays: stars
X-ray binaries
topic Hydrodynamics
Stars: winds
Outflows
Gamma-rays: stars
X-ray binaries
description Binary systems that host a massive star and a non-accreting pulsar can be powerful non-thermal emitters. The relativistic pulsar wind and the non-relativistic stellar outflows interact along the orbit, producing ultrarelativistic particles that radiate from radio to gamma rays. To properly characterize the physics of these sources, and better understand their emission and impact on the environment, careful modeling of the outflow interactions, spanning a broad range of spatial and temporal scales, is needed. Full three-dimensional approaches are very computationally expensive, but simpler approximate approaches, while still realistic at the semi-quantitative level, are available. We present here the results of calculations done with a quasi three-dimensional scheme to compute the evolution of the interacting flows in a region spanning in size up to a thousand times the size of the binary. In particular, we analyze for the first time the role of different eccentricities in the large scale evolution of the shocked flows. We find that the higher the eccentricity, the closer the flows behave like a one-side outflow, which becomes rather collimated for eccentricity values >0.75. The simulations also unveil that the pulsar and the stellar winds become fully mixed within the grid for low eccentricity systems, presenting a more stochastic behavior at large scales than in the highly eccentric systems.
publishDate 2021
dc.date.none.fl_str_mv 2021
2022
2022
2022
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/262258
url http://hdl.handle.net/10261/262258
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-105510GB-C31
http://doi.org/10.3390/universe7080277
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Multidisciplinary Digital Publishing Institute
publisher.none.fl_str_mv Multidisciplinary Digital Publishing Institute
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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