Non-thermal emission in hyper-velocity and semi-relativistic stars

Context. There is a population of runaway stars that move at extremely high speeds with respect to their surroundings. The fast motion and the stellar wind of these stars, plus the wind-medium interaction, can lead to particle acceleration and non-thermal radiation. Aims. We characterise the interac...

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Autores: Martinez, Javier Rodrigo, Del Palacio, Santiago, Bosch i Ramon, Valentí, Romero, Gustavo E.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
Repositorio:Recercat. Dipósit de la Recerca de Catalunya
OAI Identifier:oai:recercat.cat:2445/192655
Acceso en línea:https://hdl.handle.net/2445/192655
Access Level:acceso abierto
Palabra clave:Ones de xoc
Estels
Shock waves
Stars
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repository_id_str
spelling Non-thermal emission in hyper-velocity and semi-relativistic starsMartinez, Javier RodrigoDel Palacio, SantiagoBosch i Ramon, ValentíRomero, Gustavo E.Ones de xocEstelsShock wavesStarsContext. There is a population of runaway stars that move at extremely high speeds with respect to their surroundings. The fast motion and the stellar wind of these stars, plus the wind-medium interaction, can lead to particle acceleration and non-thermal radiation. Aims. We characterise the interaction between the winds of fast runaway stars and their environment, in particular to establish their potential as cosmic-ray accelerators and non-thermal emitters. Methods. We model the hydrodynamics of the interaction between the stellar wind and the surrounding material. We self-consistently calculate the injection and transport of relativistic particles in the bow shock using a multi-zone code, and compute their broadband emission from radio to γ-rays. Results. Both the forward and reverse shocks are favourable sites for particle acceleration, although the radiative efficiency of particles is low and therefore the expected fluxes are in general rather faint. Conclusions. We show that high-sensitivity observations in the radio band can be used to detect the non-thermal radiation associated with bow shocks from hyper-velocity and semi-relativistic stars. Hyper-velocity stars are expected to be modest sources of sub-TeV cosmic rays, accounting perhaps for ∼0.1% of that of galactic cosmic rays.EDP Sciences2023202320222023info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersion11 p.application/pdfhttps://hdl.handle.net/2445/192655Articles publicats en revistes (Física Quàntica i Astrofísica)reponame:Recercat. Dipósit de la Recerca de Catalunyainstname:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)InglésReproducció del document publicat a: https://doi.org/10.1051/0004-6361/202142727Astronomy & Astrophysics, 2022, vol. 661, p. 102https://doi.org/10.1051/0004-6361/202142727(c) The European Southern Observatory (ESO), 2022info:eu-repo/semantics/openAccessoai:recercat.cat:2445/1926552026-05-29T05:05:01Z
dc.title.none.fl_str_mv Non-thermal emission in hyper-velocity and semi-relativistic stars
title Non-thermal emission in hyper-velocity and semi-relativistic stars
spellingShingle Non-thermal emission in hyper-velocity and semi-relativistic stars
Martinez, Javier Rodrigo
Ones de xoc
Estels
Shock waves
Stars
title_short Non-thermal emission in hyper-velocity and semi-relativistic stars
title_full Non-thermal emission in hyper-velocity and semi-relativistic stars
title_fullStr Non-thermal emission in hyper-velocity and semi-relativistic stars
title_full_unstemmed Non-thermal emission in hyper-velocity and semi-relativistic stars
title_sort Non-thermal emission in hyper-velocity and semi-relativistic stars
dc.creator.none.fl_str_mv Martinez, Javier Rodrigo
Del Palacio, Santiago
Bosch i Ramon, Valentí
Romero, Gustavo E.
author Martinez, Javier Rodrigo
author_facet Martinez, Javier Rodrigo
Del Palacio, Santiago
Bosch i Ramon, Valentí
Romero, Gustavo E.
author_role author
author2 Del Palacio, Santiago
Bosch i Ramon, Valentí
Romero, Gustavo E.
author2_role author
author
author
dc.subject.none.fl_str_mv Ones de xoc
Estels
Shock waves
Stars
topic Ones de xoc
Estels
Shock waves
Stars
description Context. There is a population of runaway stars that move at extremely high speeds with respect to their surroundings. The fast motion and the stellar wind of these stars, plus the wind-medium interaction, can lead to particle acceleration and non-thermal radiation. Aims. We characterise the interaction between the winds of fast runaway stars and their environment, in particular to establish their potential as cosmic-ray accelerators and non-thermal emitters. Methods. We model the hydrodynamics of the interaction between the stellar wind and the surrounding material. We self-consistently calculate the injection and transport of relativistic particles in the bow shock using a multi-zone code, and compute their broadband emission from radio to γ-rays. Results. Both the forward and reverse shocks are favourable sites for particle acceleration, although the radiative efficiency of particles is low and therefore the expected fluxes are in general rather faint. Conclusions. We show that high-sensitivity observations in the radio band can be used to detect the non-thermal radiation associated with bow shocks from hyper-velocity and semi-relativistic stars. Hyper-velocity stars are expected to be modest sources of sub-TeV cosmic rays, accounting perhaps for ∼0.1% of that of galactic cosmic rays.
publishDate 2022
dc.date.none.fl_str_mv 2022
2023
2023
2023
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/2445/192655
url https://hdl.handle.net/2445/192655
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/10.1051/0004-6361/202142727
Astronomy & Astrophysics, 2022, vol. 661, p. 102
https://doi.org/10.1051/0004-6361/202142727
dc.rights.none.fl_str_mv (c) The European Southern Observatory (ESO), 2022
info:eu-repo/semantics/openAccess
rights_invalid_str_mv (c) The European Southern Observatory (ESO), 2022
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv 11 p.
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:Recercat. Dipósit de la Recerca de Catalunya
instname:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
instname_str Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
reponame_str Recercat. Dipósit de la Recerca de Catalunya
collection Recercat. Dipósit de la Recerca de Catalunya
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,811543

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