Runaway stars as cosmic ray injectors inside molecular clouds

Giant molecular clouds (GMCs) are a new population of gamma-ray sources, being the target of cosmic rays (CRs) - locally accelerated or not. These clouds host very young stellar clusters where massive star formation takes place. Eventually, some of the stars are ejected from the clusters, becoming r...

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Detalles Bibliográficos
Autores: Valle, María Victoria del, Romero, Gustavo Esteban, Santos-Lima, R.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2015
País:Argentina
Institución:Universidad Nacional de La Plata
Repositorio:SEDICI (UNLP)
Idioma:inglés
OAI Identifier:oai:sedici.unlp.edu.ar:10915/85939
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/85939
Access Level:acceso abierto
Palabra clave:Ciencias Astronómicas
Cosmic rays
Gamma-rays: ISM
ISM: clouds
Radiation mechanisms: non-thermal
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spelling Runaway stars as cosmic ray injectors inside molecular cloudsValle, María Victoria delRomero, Gustavo EstebanSantos-Lima, R.Ciencias AstronómicasCosmic raysGamma-rays: ISMISM: cloudsRadiation mechanisms: non-thermalGiant molecular clouds (GMCs) are a new population of gamma-ray sources, being the target of cosmic rays (CRs) - locally accelerated or not. These clouds host very young stellar clusters where massive star formation takes place. Eventually, some of the stars are ejected from the clusters, becoming runaway stars. These stars move supersonically through the cloud and develop bowshocks where particles can be accelerated up to relativistic energies. As a result, the bowshocks present non-thermal emission, and inject relativistic protons in the cloud. These protons diffuse in theGMCinteracting with the matter.We present a model for the non-thermal radiation generated by protons and secondary pairs accelerated in the bowshocks of massive runaway stars within young GMCs. We solve the transport equation for primary protons and secondary pairs as the stars move through the cloud.We present non-thermal emissivity maps in radio and in gamma-rays as a function of time. We obtain X-ray luminosities of the order of ~1032 erg s-1 and gamma-ray luminosities ~1034 erg s-1. We conclude that, under some assumptions, relativistic protons from massive runaway stars interacting with matter in GMCs give rise to extended non-thermal sources.Facultad de Ciencias Astronómicas y Geofísicas2015info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf207-220http://sedici.unlp.edu.ar/handle/10915/85939enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stu2732info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2024-05-08T12:54:55Zoai:sedici.unlp.edu.ar:10915/85939Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292024-05-08 12:54:56.103SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Runaway stars as cosmic ray injectors inside molecular clouds
title Runaway stars as cosmic ray injectors inside molecular clouds
spellingShingle Runaway stars as cosmic ray injectors inside molecular clouds
Valle, María Victoria del
Ciencias Astronómicas
Cosmic rays
Gamma-rays: ISM
ISM: clouds
Radiation mechanisms: non-thermal
title_short Runaway stars as cosmic ray injectors inside molecular clouds
title_full Runaway stars as cosmic ray injectors inside molecular clouds
title_fullStr Runaway stars as cosmic ray injectors inside molecular clouds
title_full_unstemmed Runaway stars as cosmic ray injectors inside molecular clouds
title_sort Runaway stars as cosmic ray injectors inside molecular clouds
dc.creator.none.fl_str_mv Valle, María Victoria del
Romero, Gustavo Esteban
Santos-Lima, R.
author Valle, María Victoria del
author_facet Valle, María Victoria del
Romero, Gustavo Esteban
Santos-Lima, R.
author_role author
author2 Romero, Gustavo Esteban
Santos-Lima, R.
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Cosmic rays
Gamma-rays: ISM
ISM: clouds
Radiation mechanisms: non-thermal
topic Ciencias Astronómicas
Cosmic rays
Gamma-rays: ISM
ISM: clouds
Radiation mechanisms: non-thermal
description Giant molecular clouds (GMCs) are a new population of gamma-ray sources, being the target of cosmic rays (CRs) - locally accelerated or not. These clouds host very young stellar clusters where massive star formation takes place. Eventually, some of the stars are ejected from the clusters, becoming runaway stars. These stars move supersonically through the cloud and develop bowshocks where particles can be accelerated up to relativistic energies. As a result, the bowshocks present non-thermal emission, and inject relativistic protons in the cloud. These protons diffuse in theGMCinteracting with the matter.We present a model for the non-thermal radiation generated by protons and secondary pairs accelerated in the bowshocks of massive runaway stars within young GMCs. We solve the transport equation for primary protons and secondary pairs as the stars move through the cloud.We present non-thermal emissivity maps in radio and in gamma-rays as a function of time. We obtain X-ray luminosities of the order of ~1032 erg s-1 and gamma-ray luminosities ~1034 erg s-1. We conclude that, under some assumptions, relativistic protons from massive runaway stars interacting with matter in GMCs give rise to extended non-thermal sources.
publishDate 2015
dc.date.none.fl_str_mv 2015
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/85939
url http://sedici.unlp.edu.ar/handle/10915/85939
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0035-8711
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stu2732
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
207-220
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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