Mass-loading of bow shock pulsar wind nebulae

Autores
Morlino, Giovanni; Lyutikov, Maxim; Vorster, Michael
Año de publicación
2015
Idioma
inglés
Tipo de recurso
documento de conferencia
Estado
versión publicada
Descripción
We investigate the dynamics of bow shock nebulae created by pulsars moving supersonically through a partially ionized interstellar medium. A fraction of interstellar neutral hydrogen atoms penetrating into the tail region of a pulsar wind will undergo photo-ionization due to the UV light emitted by the nebula, with the resulting mass loading dramatically changing the flow dynamics of the light leptonic pulsar wind. Using a quasi 1-D hydrodynamic model of relativistic flow we find that if a relatively small density of neutral hydrogen, as low as 10⁻⁴ cm⁻³, penetrate inside the pulsar wind, this is sufficient to strongly affect the tail flow. Mass loading leads to the fast expansion of the pulsar wind tail, making the tail flow intrinsically non-stationary. The shapes predicted for the bow shock nebulae compare well with observations, both in Hα and X-rays.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
bow shock nebulae
pulsars
ionized interstellar medium
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/167940
Acceder
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oai_identifier_str oai:sedici.unlp.edu.ar:10915/167940
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repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Mass-loading of bow shock pulsar wind nebulaeMorlino, GiovanniLyutikov, MaximVorster, MichaelCiencias Astronómicasbow shock nebulaepulsarsionized interstellar mediumWe investigate the dynamics of bow shock nebulae created by pulsars moving supersonically through a partially ionized interstellar medium. A fraction of interstellar neutral hydrogen atoms penetrating into the tail region of a pulsar wind will undergo photo-ionization due to the UV light emitted by the nebula, with the resulting mass loading dramatically changing the flow dynamics of the light leptonic pulsar wind. Using a quasi 1-D hydrodynamic model of relativistic flow we find that if a relatively small density of neutral hydrogen, as low as 10⁻⁴ cm⁻³, penetrate inside the pulsar wind, this is sufficient to strongly affect the tail flow. Mass loading leads to the fast expansion of the pulsar wind tail, making the tail flow intrinsically non-stationary. The shapes predicted for the bow shock nebulae compare well with observations, both in Hα and X-rays.Facultad de Ciencias Astronómicas y Geofísicas2015-10info:eu-repo/semantics/conferenceObjectinfo:eu-repo/semantics/publishedVersionObjeto de conferenciahttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdf73-80http://sedici.unlp.edu.ar/handle/10915/167940enginfo:eu-repo/semantics/altIdentifier/isbn/978-987-24948-3-4info:eu-repo/semantics/reference/url/https://sedici.unlp.edu.ar/handle/10915/167830info: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:UNLP2025-10-22T17:25:39Zoai:sedici.unlp.edu.ar:10915/167940Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-22 17:25:39.362SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Mass-loading of bow shock pulsar wind nebulae
title Mass-loading of bow shock pulsar wind nebulae
spellingShingle Mass-loading of bow shock pulsar wind nebulae
Morlino, Giovanni
Ciencias Astronómicas
bow shock nebulae
pulsars
ionized interstellar medium
title_short Mass-loading of bow shock pulsar wind nebulae
title_full Mass-loading of bow shock pulsar wind nebulae
title_fullStr Mass-loading of bow shock pulsar wind nebulae
title_full_unstemmed Mass-loading of bow shock pulsar wind nebulae
title_sort Mass-loading of bow shock pulsar wind nebulae
dc.creator.none.fl_str_mv Morlino, Giovanni
Lyutikov, Maxim
Vorster, Michael
author Morlino, Giovanni
author_facet Morlino, Giovanni
Lyutikov, Maxim
Vorster, Michael
author_role author
author2 Lyutikov, Maxim
Vorster, Michael
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
bow shock nebulae
pulsars
ionized interstellar medium
topic Ciencias Astronómicas
bow shock nebulae
pulsars
ionized interstellar medium
dc.description.none.fl_txt_mv We investigate the dynamics of bow shock nebulae created by pulsars moving supersonically through a partially ionized interstellar medium. A fraction of interstellar neutral hydrogen atoms penetrating into the tail region of a pulsar wind will undergo photo-ionization due to the UV light emitted by the nebula, with the resulting mass loading dramatically changing the flow dynamics of the light leptonic pulsar wind. Using a quasi 1-D hydrodynamic model of relativistic flow we find that if a relatively small density of neutral hydrogen, as low as 10⁻⁴ cm⁻³, penetrate inside the pulsar wind, this is sufficient to strongly affect the tail flow. Mass loading leads to the fast expansion of the pulsar wind tail, making the tail flow intrinsically non-stationary. The shapes predicted for the bow shock nebulae compare well with observations, both in Hα and X-rays.
Facultad de Ciencias Astronómicas y Geofísicas
description We investigate the dynamics of bow shock nebulae created by pulsars moving supersonically through a partially ionized interstellar medium. A fraction of interstellar neutral hydrogen atoms penetrating into the tail region of a pulsar wind will undergo photo-ionization due to the UV light emitted by the nebula, with the resulting mass loading dramatically changing the flow dynamics of the light leptonic pulsar wind. Using a quasi 1-D hydrodynamic model of relativistic flow we find that if a relatively small density of neutral hydrogen, as low as 10⁻⁴ cm⁻³, penetrate inside the pulsar wind, this is sufficient to strongly affect the tail flow. Mass loading leads to the fast expansion of the pulsar wind tail, making the tail flow intrinsically non-stationary. The shapes predicted for the bow shock nebulae compare well with observations, both in Hα and X-rays.
publishDate 2015
dc.date.none.fl_str_mv 2015-10
dc.type.none.fl_str_mv info:eu-repo/semantics/conferenceObject
info:eu-repo/semantics/publishedVersion
Objeto de conferencia
http://purl.org/coar/resource_type/c_5794
info:ar-repo/semantics/documentoDeConferencia
format conferenceObject
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/167940
url http://sedici.unlp.edu.ar/handle/10915/167940
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/isbn/978-987-24948-3-4
info:eu-repo/semantics/reference/url/https://sedici.unlp.edu.ar/handle/10915/167830
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
73-80
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
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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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