On the relevance of chaos for halo stars in the solar neighbourhood
- Autores
- Maffione, Nicolas Pablo; Gomez, F. A.; Cincotta, Pablo Miguel; Giordano, Claudia Marcela; Cooper, A. P.; O'Shea, B. W.
- Año de publicación
- 2015
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We show that diffusion due to chaotic mixing in the neighbourhood of the Sun may not be as relevant as previously suggested in erasing phase space signatures of past Galactic accretion events. For this purpose, we analyse solar neighbourhood-like volumes extracted from cosmological simulations that naturally account for chaotic orbital behaviour induced by the strongly triaxial and cuspy shape of the resulting dark matter haloes, among other factors. In the approximation of an analytical static triaxial model, our results show that a large fraction of stellar halo particles in such local volumes have chaos onset times (i.e. the time-scale at which stars commonly associated with chaotic orbits will exhibit their chaotic behaviour) significantly larger than a Hubble time. Furthermore, particles that do present a chaotic behaviour within a Hubble time do not exhibit significant diffusion in phase space.
Fil: Maffione, Nicolas Pablo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina
Fil: Gomez, F. A.. Max-Planck-Institut fur Astrophysik; Alemania
Fil: Cincotta, Pablo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Giordano, Claudia Marcela . Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Cooper, A. P. . University Of Durham; Reino Unido
Fil: O'Shea, B. W.. Michigan State University; Estados Unidos - Materia
-
Chaos
Difffusion
Numerical methods
Evolution of the Galaxy
Galaxy - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/13886
Ver los metadatos del registro completo
id |
CONICETDig_59a8fe3284b8b589fc60e92a2f180afc |
---|---|
oai_identifier_str |
oai:ri.conicet.gov.ar:11336/13886 |
network_acronym_str |
CONICETDig |
repository_id_str |
3498 |
network_name_str |
CONICET Digital (CONICET) |
spelling |
On the relevance of chaos for halo stars in the solar neighbourhoodMaffione, Nicolas PabloGomez, F. A.Cincotta, Pablo MiguelGiordano, Claudia Marcela Cooper, A. P. O'Shea, B. W.ChaosDifffusionNumerical methodsEvolution of the GalaxyGalaxyhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We show that diffusion due to chaotic mixing in the neighbourhood of the Sun may not be as relevant as previously suggested in erasing phase space signatures of past Galactic accretion events. For this purpose, we analyse solar neighbourhood-like volumes extracted from cosmological simulations that naturally account for chaotic orbital behaviour induced by the strongly triaxial and cuspy shape of the resulting dark matter haloes, among other factors. In the approximation of an analytical static triaxial model, our results show that a large fraction of stellar halo particles in such local volumes have chaos onset times (i.e. the time-scale at which stars commonly associated with chaotic orbits will exhibit their chaotic behaviour) significantly larger than a Hubble time. Furthermore, particles that do present a chaotic behaviour within a Hubble time do not exhibit significant diffusion in phase space.Fil: Maffione, Nicolas Pablo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; ArgentinaFil: Gomez, F. A.. Max-Planck-Institut fur Astrophysik; AlemaniaFil: Cincotta, Pablo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Giordano, Claudia Marcela . Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Cooper, A. P. . University Of Durham; Reino UnidoFil: O'Shea, B. W.. Michigan State University; Estados UnidosOxford University Press2015-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/13886Maffione, Nicolas Pablo; Gomez, F. A.; Cincotta, Pablo Miguel; Giordano, Claudia Marcela ; Cooper, A. P. ; et al.; On the relevance of chaos for halo stars in the solar neighbourhood; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 453; 3; 9-2015; 2830-28470035-8711enginfo:eu-repo/semantics/altIdentifier/arxiv/http://arxiv.org/abs/1508.00579info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv1778info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stv1778info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:34:24Zoai:ri.conicet.gov.ar:11336/13886instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:34:24.723CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
On the relevance of chaos for halo stars in the solar neighbourhood |
title |
On the relevance of chaos for halo stars in the solar neighbourhood |
spellingShingle |
On the relevance of chaos for halo stars in the solar neighbourhood Maffione, Nicolas Pablo Chaos Difffusion Numerical methods Evolution of the Galaxy Galaxy |
title_short |
On the relevance of chaos for halo stars in the solar neighbourhood |
title_full |
On the relevance of chaos for halo stars in the solar neighbourhood |
title_fullStr |
On the relevance of chaos for halo stars in the solar neighbourhood |
title_full_unstemmed |
On the relevance of chaos for halo stars in the solar neighbourhood |
title_sort |
On the relevance of chaos for halo stars in the solar neighbourhood |
dc.creator.none.fl_str_mv |
Maffione, Nicolas Pablo Gomez, F. A. Cincotta, Pablo Miguel Giordano, Claudia Marcela Cooper, A. P. O'Shea, B. W. |
author |
Maffione, Nicolas Pablo |
author_facet |
Maffione, Nicolas Pablo Gomez, F. A. Cincotta, Pablo Miguel Giordano, Claudia Marcela Cooper, A. P. O'Shea, B. W. |
author_role |
author |
author2 |
Gomez, F. A. Cincotta, Pablo Miguel Giordano, Claudia Marcela Cooper, A. P. O'Shea, B. W. |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
Chaos Difffusion Numerical methods Evolution of the Galaxy Galaxy |
topic |
Chaos Difffusion Numerical methods Evolution of the Galaxy Galaxy |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
We show that diffusion due to chaotic mixing in the neighbourhood of the Sun may not be as relevant as previously suggested in erasing phase space signatures of past Galactic accretion events. For this purpose, we analyse solar neighbourhood-like volumes extracted from cosmological simulations that naturally account for chaotic orbital behaviour induced by the strongly triaxial and cuspy shape of the resulting dark matter haloes, among other factors. In the approximation of an analytical static triaxial model, our results show that a large fraction of stellar halo particles in such local volumes have chaos onset times (i.e. the time-scale at which stars commonly associated with chaotic orbits will exhibit their chaotic behaviour) significantly larger than a Hubble time. Furthermore, particles that do present a chaotic behaviour within a Hubble time do not exhibit significant diffusion in phase space. Fil: Maffione, Nicolas Pablo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina Fil: Gomez, F. A.. Max-Planck-Institut fur Astrophysik; Alemania Fil: Cincotta, Pablo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Giordano, Claudia Marcela . Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Cooper, A. P. . University Of Durham; Reino Unido Fil: O'Shea, B. W.. Michigan State University; Estados Unidos |
description |
We show that diffusion due to chaotic mixing in the neighbourhood of the Sun may not be as relevant as previously suggested in erasing phase space signatures of past Galactic accretion events. For this purpose, we analyse solar neighbourhood-like volumes extracted from cosmological simulations that naturally account for chaotic orbital behaviour induced by the strongly triaxial and cuspy shape of the resulting dark matter haloes, among other factors. In the approximation of an analytical static triaxial model, our results show that a large fraction of stellar halo particles in such local volumes have chaos onset times (i.e. the time-scale at which stars commonly associated with chaotic orbits will exhibit their chaotic behaviour) significantly larger than a Hubble time. Furthermore, particles that do present a chaotic behaviour within a Hubble time do not exhibit significant diffusion in phase space. |
publishDate |
2015 |
dc.date.none.fl_str_mv |
2015-09 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion 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://hdl.handle.net/11336/13886 Maffione, Nicolas Pablo; Gomez, F. A.; Cincotta, Pablo Miguel; Giordano, Claudia Marcela ; Cooper, A. P. ; et al.; On the relevance of chaos for halo stars in the solar neighbourhood; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 453; 3; 9-2015; 2830-2847 0035-8711 |
url |
http://hdl.handle.net/11336/13886 |
identifier_str_mv |
Maffione, Nicolas Pablo; Gomez, F. A.; Cincotta, Pablo Miguel; Giordano, Claudia Marcela ; Cooper, A. P. ; et al.; On the relevance of chaos for halo stars in the solar neighbourhood; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 453; 3; 9-2015; 2830-2847 0035-8711 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/arxiv/http://arxiv.org/abs/1508.00579 info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv1778 info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stv1778 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
Oxford University Press |
publisher.none.fl_str_mv |
Oxford University Press |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
reponame_str |
CONICET Digital (CONICET) |
collection |
CONICET Digital (CONICET) |
instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
_version_ |
1844614360939364352 |
score |
13.070432 |