A model for high-mass microquasar jets under the influence of a strong stellar wind

Context. High-mass microquasars (HMMQs) are systems from which relativistic jets are launched. At the scales of several times the binary system size, the jets are expected to follow a helical path caused by the interaction with a strong stellar wind and orbital motion.Such a trajectory has its influ...

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Detalles Bibliográficos
Autores: Molina, Edgar, Del Palacio, S., Bosch i Ramon, Valentí
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2019
País:España
Institución:Universidad de Barcelona
Repositorio:Dipòsit Digital de la UB
OAI Identifier:oai:diposit.ub.edu:2445/161246
Acceso en línea:https://hdl.handle.net/2445/161246
Access Level:acceso abierto
Palabra clave:Raigs gamma
Estels binaris de raigs X
Gamma rays
X-ray binaries
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oai_identifier_str oai:diposit.ub.edu:2445/161246
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repository_id_str
spelling A model for high-mass microquasar jets under the influence of a strong stellar windMolina, EdgarDel Palacio, S.Bosch i Ramon, ValentíRaigs gammaEstels binaris de raigs XGamma raysX-ray binariesContext. High-mass microquasars (HMMQs) are systems from which relativistic jets are launched. At the scales of several times the binary system size, the jets are expected to follow a helical path caused by the interaction with a strong stellar wind and orbital motion.Such a trajectory has its influence on the non-thermal emission of the jets, which also depends strongly on the observing angle due to Doppler boosting effects. Aims. We explore how the expected non-thermal emission of HMMQ jets at small scales is affected by the impact of the stellar wind and the orbital motion on the jet propagation. Methods. We studied the broadband non-thermal emission, from radio to gamma rays, produced in HMMQ jets up to a distance of several orbital separations, taking into account a realistic jet trajectory, different model parameters, and orbital modulation. The jet trajectory is computed by considering momentum transfer with the stellar wind. Electrons are injected at the position where a recollimation shock in the jets is expected due to the wind impact. Their distribution along the jet path is obtained assuming local acceleration at the recollimation shock, and cooling via adiabatic, synchrotron, and inverse Compton processes. The synchrotron and inverse Compton emission is calculated taking into account synchrotron self-absorption within the jet, free-free absorption with the stellar wind, and absorption by stellar photons via pair production. Results. The spectrum is totally dominated by the jet over the counter-jet due to Doppler boosting. Broadband emission from microwaves to gamma rays is predicted, with radio emission being totally absorbed. This emission is rather concentrated in the regions close to the binary system and features strong orbital modulation at high energies. Asymmetric light curves are obtained owing to the helical trajectory of the jets. Conclusions. The presence of helical shaped jets could be inferred from asymmetries in the light curves, which become noticeable only for large jet Lorentz factors and low magnetic fields. Model parameters could be constrained if accurate phase-resolved lightcurves from GeV to TeV energies were available. The predictions for the synchrotron and the inverse Compton radiation are quite sensitive of the parameters determining the wind-jet interaction structure.EDP Sciences2019info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionapplication/pdfhttps://hdl.handle.net/2445/161246Articles publicats en revistes (Física Quàntica i Astrofísica)reponame:Dipòsit Digital de la UBinstname:Universidad de BarcelonaInglésReproducció del document publicat a: https://doi.org/10.1051/0004-6361/201935960Astronomy & Astrophysics, 2019, vol. 629, p. A129https://doi.org/10.1051/0004-6361/201935960(c) The European Southern Observatory (ESO), 2019info:eu-repo/semantics/openAccessoai:diposit.ub.edu:2445/1612462026-05-27T06:46:51Z
dc.title.none.fl_str_mv A model for high-mass microquasar jets under the influence of a strong stellar wind
title A model for high-mass microquasar jets under the influence of a strong stellar wind
spellingShingle A model for high-mass microquasar jets under the influence of a strong stellar wind
Molina, Edgar
Raigs gamma
Estels binaris de raigs X
Gamma rays
X-ray binaries
title_short A model for high-mass microquasar jets under the influence of a strong stellar wind
title_full A model for high-mass microquasar jets under the influence of a strong stellar wind
title_fullStr A model for high-mass microquasar jets under the influence of a strong stellar wind
title_full_unstemmed A model for high-mass microquasar jets under the influence of a strong stellar wind
title_sort A model for high-mass microquasar jets under the influence of a strong stellar wind
dc.creator.none.fl_str_mv Molina, Edgar
Del Palacio, S.
Bosch i Ramon, Valentí
author Molina, Edgar
author_facet Molina, Edgar
Del Palacio, S.
Bosch i Ramon, Valentí
author_role author
author2 Del Palacio, S.
Bosch i Ramon, Valentí
author2_role author
author
dc.subject.none.fl_str_mv Raigs gamma
Estels binaris de raigs X
Gamma rays
X-ray binaries
topic Raigs gamma
Estels binaris de raigs X
Gamma rays
X-ray binaries
description Context. High-mass microquasars (HMMQs) are systems from which relativistic jets are launched. At the scales of several times the binary system size, the jets are expected to follow a helical path caused by the interaction with a strong stellar wind and orbital motion.Such a trajectory has its influence on the non-thermal emission of the jets, which also depends strongly on the observing angle due to Doppler boosting effects. Aims. We explore how the expected non-thermal emission of HMMQ jets at small scales is affected by the impact of the stellar wind and the orbital motion on the jet propagation. Methods. We studied the broadband non-thermal emission, from radio to gamma rays, produced in HMMQ jets up to a distance of several orbital separations, taking into account a realistic jet trajectory, different model parameters, and orbital modulation. The jet trajectory is computed by considering momentum transfer with the stellar wind. Electrons are injected at the position where a recollimation shock in the jets is expected due to the wind impact. Their distribution along the jet path is obtained assuming local acceleration at the recollimation shock, and cooling via adiabatic, synchrotron, and inverse Compton processes. The synchrotron and inverse Compton emission is calculated taking into account synchrotron self-absorption within the jet, free-free absorption with the stellar wind, and absorption by stellar photons via pair production. Results. The spectrum is totally dominated by the jet over the counter-jet due to Doppler boosting. Broadband emission from microwaves to gamma rays is predicted, with radio emission being totally absorbed. This emission is rather concentrated in the regions close to the binary system and features strong orbital modulation at high energies. Asymmetric light curves are obtained owing to the helical trajectory of the jets. Conclusions. The presence of helical shaped jets could be inferred from asymmetries in the light curves, which become noticeable only for large jet Lorentz factors and low magnetic fields. Model parameters could be constrained if accurate phase-resolved lightcurves from GeV to TeV energies were available. The predictions for the synchrotron and the inverse Compton radiation are quite sensitive of the parameters determining the wind-jet interaction structure.
publishDate 2019
dc.date.none.fl_str_mv 2019
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv https://hdl.handle.net/2445/161246
url https://hdl.handle.net/2445/161246
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv Reproducció del document publicat a: https://doi.org/10.1051/0004-6361/201935960
Astronomy & Astrophysics, 2019, vol. 629, p. A129
https://doi.org/10.1051/0004-6361/201935960
dc.rights.none.fl_str_mv (c) The European Southern Observatory (ESO), 2019
info:eu-repo/semantics/openAccess
rights_invalid_str_mv (c) The European Southern Observatory (ESO), 2019
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv Articles publicats en revistes (Física Quàntica i Astrofísica)
reponame:Dipòsit Digital de la UB
instname:Universidad de Barcelona
instname_str Universidad de Barcelona
reponame_str Dipòsit Digital de la UB
collection Dipòsit Digital de la UB
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15.301629

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