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Campo DC | Valor | Lengua/Idioma |
---|---|---|
dc.contributor.author | Maffione, Nicolás Pablo | - |
dc.contributor.author | Gómez, Facundo A. | - |
dc.contributor.author | Cincotta, Pablo M. | - |
dc.contributor.author | Giordano, Claudia M. | - |
dc.contributor.author | Grand, Robert J. | - |
dc.contributor.author | Marinacci, Federico | - |
dc.contributor.author | Pakmor, Rudiger | - |
dc.contributor.author | Simpson, Christine M. | - |
dc.contributor.author | Springel, Volker | - |
dc.contributor.author | Frenk, Carlos | - |
dc.date.accessioned | 2019-11-25T13:23:36Z | - |
dc.date.available | 2019-11-25T13:23:36Z | - |
dc.date.issued | 2018-05-17 | - |
dc.identifier.citation | Maffione, 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); 4052-4067 | es_ES |
dc.identifier.issn | 0035-8711 | es_ES |
dc.identifier.issn | 1365-2966 | es_ES |
dc.identifier.uri | https://rid.unrn.edu.ar/jspui/handle/20.500.12049/3762 | - |
dc.description.abstract | In 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.extent | p. 4052-4067 | es_ES |
dc.format.medium | impreso | es_ES |
dc.format.medium | digital | es_ES |
dc.language.iso | en | es_ES |
dc.publisher | Oxford University Press | es_ES |
dc.title | On the relevance of chaos for halo stars in the solar neighbourhood II | es_ES |
dc.type | Articulo | es_ES |
dc.rights.license | https://creativecommons.org/licenses/by-nc-sa/4.0/ | es_ES |
dc.description.filiation | Fil: 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.filiation | Fil: Gómez, Facundo A. Universidad de La Serena. Departamento de Física y Astronomía; Chile. | es_ES |
dc.description.filiation | Fil: 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.filiation | Fil: 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.filiation | Fil: Grand, Robert J. Heidelberger Institut fur Theoretische Studien; Alemania. | es_ES |
dc.description.filiation | Fil: Marinacci, Federico. MIT. Kavli Institute for Astrophysics and Space Researc. Department of Physics; USA. | es_ES |
dc.description.filiation | Fil: Pakmor, Rudiger. Heidelberger Institut fur Theoretische Studien; Alemania | es_ES |
dc.description.filiation | Fil: Simpson, Christine M. Heidelberger Institut fur Theoretische Studien; Alemania | es_ES |
dc.description.filiation | Fil: Springel, Volker. Max Planck Institut for Astrophysik; Alemania | es_ES |
dc.description.filiation | Fil: Frenk, Carlos. Durham University. Institute for Computational Cosmology. Department of Physics; UK. | es_ES |
dc.description.filiation | Fil: Maffione, Nicolás P. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina | es_ES |
dc.description.filiation | Fil: Gómez, Facundo A. Universidad de La Serena. Instituto de Investigación Multidisciplinar en Ciencia y Tecnología; Chile | es_ES |
dc.description.filiation | Fil: Gómez, Facundo A. Max Planck Institute for Astrophysics; Alemania | es_ES |
dc.description.filiation | Fil: Cincotta, Pablo M. Universidad Nacional de La Plata. Instituto de Astrofísica de La Plata. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina | es_ES |
dc.description.filiation | Fil: Giordano, Claudia M. Universidad Nacional de La Plata. Instituto de Astrofísica de La Plata. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina | es_ES |
dc.description.filiation | Fil: Grand, Robert J. Zentrum fur Astronomie der Universitat Heidelberg. Astronomisches Rechen institut; Alemania | es_ES |
dc.description.filiation | Fil: Springel, Volker. Heidelberger Institut fur Theoretische Studien; Alemania. | es_ES |
dc.description.filiation | Fil: Springel, Volker. Zentrum fur Astronomie der Universitat Heidelberg. Astronomisches Rechen institut; Alemania | es_ES |
dc.subject.keyword | Chaos | es_ES |
dc.subject.keyword | diffusion | es_ES |
dc.subject.keyword | Methods: Numerical | es_ES |
dc.subject.keyword | Galaxy: Evolution | es_ES |
dc.type.version | info:eu-repo/semantics/acceptedVersion | es_ES |
dc.origin.lugarDesarrollo | Universidad Nacional de Río Negro | es_ES |
dc.origin.lugarDesarrollo | Max-Planck-Institut fur Astrophysik | es_ES |
dc.relation.journalissue | 478 (3) | es_ES |
dc.description.review | true | es_ES |
dc.description.resumen | In 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.doi | https://doi.org/10.1093/mnras/sty1297 | - |
dc.relation.journalTitle | Monthly Notices of the Royal Astronomical Society | es_ES |
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