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dc.contributor.authorMaffione, Nicolás Pablo-
dc.contributor.authorGómez, Facundo A.-
dc.contributor.authorCincotta, Pablo M.-
dc.contributor.authorGiordano, Claudia M.-
dc.contributor.authorGrand, Robert J.-
dc.contributor.authorMarinacci, Federico-
dc.contributor.authorPakmor, Rudiger-
dc.contributor.authorSimpson, Christine M.-
dc.contributor.authorSpringel, Volker-
dc.contributor.authorFrenk, Carlos-
dc.date.accessioned2019-11-25T13:23:36Z-
dc.date.available2019-11-25T13:23:36Z-
dc.date.issued2018-05-17-
dc.identifier.citationMaffione, Nicolas P., Gomez, Facundo A., Cincotta, Pablo M., Giordano, Claudia M., Grand, Robert J., y et al. (2018). On the relevance of chaos for halo stars in the solar neighbourhood II. Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 478 (3); 4052-4067es_ES
dc.identifier.issn0035-8711es_ES
dc.identifier.issn1365-2966es_ES
dc.identifier.urihttps://rid.unrn.edu.ar/jspui/handle/20.500.12049/3762-
dc.description.abstractIn a previous paper based on dark matter only simulations we show that, in the approximation of an analytic and static potential describing the strongly triaxial and cuspy shape of Milky Way-sized haloes, diffusion due to chaotic mixing in the neighbourhood of the Sun does not efficiently erase phase space signatures of past accretion events. In this second paper we further explore the effect of chaotic mixing using multicomponent Galactic potential models and solar neighbourhood-like volumes extracted from fully cosmological hydrodynamic simulations, thus naturally accounting for the gravitational potential associated with baryonic components, such as the bulge and disc. Despite the strong change in the global Galactic potentials with respect to those obtained in dark matter only simulations, our results confirm that a large fraction of halo particles evolving on chaotic orbits exhibit their chaotic behaviour after periods of time significantly larger than a Hubble time. In addition, significant diffusion in phase space is not observed on those particles that do exhibit chaotic behaviour within a Hubble time.es_ES
dc.format.extentp. 4052-4067es_ES
dc.format.mediumimpresoes_ES
dc.format.mediumdigitales_ES
dc.language.isoenes_ES
dc.publisherOxford University Presses_ES
dc.titleOn the relevance of chaos for halo stars in the solar neighbourhood IIes_ES
dc.typeArticuloes_ES
dc.rights.licensehttps://creativecommons.org/licenses/by-nc-sa/4.0/es_ES
dc.description.filiationFil: Maffione, Nicolás P. Universidad Nacional de Río Negro. Sede Antina. Laboratorio de Procesamiento de Señales Aplicadas y Computación de Alto Rendimiento; Argentina.es_ES
dc.description.filiationFil: Gómez, Facundo A. Universidad de La Serena. Departamento de Física y Astronomía; Chile.es_ES
dc.description.filiationFil: Cincotta, Pablo M. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Grupo de Caos en Sistemas Hamiltonianos; Argentina.es_ES
dc.description.filiationFil: Giordano, Claudia M. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Grupo de Caos en Sistemas Hamiltonianos; Argentina.es_ES
dc.description.filiationFil: Grand, Robert J. Heidelberger Institut fur Theoretische Studien; Alemania.es_ES
dc.description.filiationFil: Marinacci, Federico. MIT. Kavli Institute for Astrophysics and Space Researc. Department of Physics; USA.es_ES
dc.description.filiationFil: Pakmor, Rudiger. Heidelberger Institut fur Theoretische Studien; Alemaniaes_ES
dc.description.filiationFil: Simpson, Christine M. Heidelberger Institut fur Theoretische Studien; Alemaniaes_ES
dc.description.filiationFil: Springel, Volker. Max Planck Institut for Astrophysik; Alemaniaes_ES
dc.description.filiationFil: Frenk, Carlos. Durham University. Institute for Computational Cosmology. Department of Physics; UK.es_ES
dc.description.filiationFil: Maffione, Nicolás P. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentinaes_ES
dc.description.filiationFil: Gómez, Facundo A. Universidad de La Serena. Instituto de Investigación Multidisciplinar en Ciencia y Tecnología; Chilees_ES
dc.description.filiationFil: Gómez, Facundo A. Max Planck Institute for Astrophysics; Alemaniaes_ES
dc.description.filiationFil: Cincotta, Pablo M. Universidad Nacional de La Plata. Instituto de Astrofísica de La Plata. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentinaes_ES
dc.description.filiationFil: Giordano, Claudia M. Universidad Nacional de La Plata. Instituto de Astrofísica de La Plata. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentinaes_ES
dc.description.filiationFil: Grand, Robert J. Zentrum fur Astronomie der Universitat Heidelberg. Astronomisches Rechen institut; Alemaniaes_ES
dc.description.filiationFil: Springel, Volker. Heidelberger Institut fur Theoretische Studien; Alemania.es_ES
dc.description.filiationFil: Springel, Volker. Zentrum fur Astronomie der Universitat Heidelberg. Astronomisches Rechen institut; Alemaniaes_ES
dc.subject.keywordChaoses_ES
dc.subject.keyworddiffusiones_ES
dc.subject.keywordMethods: Numericales_ES
dc.subject.keywordGalaxy: Evolutiones_ES
dc.type.versioninfo:eu-repo/semantics/acceptedVersiones_ES
dc.origin.lugarDesarrolloUniversidad Nacional de Río Negroes_ES
dc.origin.lugarDesarrolloMax-Planck-Institut fur Astrophysikes_ES
dc.relation.journalissue478 (3)es_ES
dc.description.reviewtruees_ES
dc.description.resumenIn a previous paper based on dark matter only simulations we show that, in the approximation of an analytic and static potential describing the strongly triaxial and cuspy shape of Milky Way-sized haloes, diffusion due to chaotic mixing in the neighbourhood of the Sun does not efficiently erase phase space signatures of past accretion events. In this second paper we further explore the effect of chaotic mixing using multicomponent Galactic potential models and solar neighbourhood-like volumes extracted from fully cosmological hydrodynamic simulations, thus naturally accounting for the gravitational potential associated with baryonic components, such as the bulge and disc. Despite the strong change in the global Galactic potentials with respect to those obtained in dark matter only simulations, our results confirm that a large fraction of halo particles evolving on chaotic orbits exhibit their chaotic behaviour after periods of time significantly larger than a Hubble time. In addition, significant diffusion in phase space is not observed on those particles that do exhibit chaotic behaviour within a Hubble time.es_ES
dc.identifier.doihttps://doi.org/10.1093/mnras/sty1297-
dc.relation.journalTitleMonthly Notices of the Royal Astronomical Societyes_ES
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