On the relevance of chaos for halo stars in the solar neighbourhood II

• Autores: Maffione, Nicolás Pablo; Gómez, Facundo A.; Cincotta, Pablo M.; Giordano, Claudia M.; Grand, Robert J.; Marinacci, Federico; Pakmor, Rudiger; Simpson, Christine M.; Springel, Volker; Frenk, Carlos
• Año de publicación: 2018
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: Chaos; diffusion; Methods: Numerical; Galaxy: Evolution
• Institución: Universidad Nacional de Río Negro

Fil: Maffione, Nicolás P. Universidad Nacional de Río Negro. Sede Antina. Laboratorio de Procesamiento de Señales Aplicadas y Computación de Alto Rendimiento; Argentina.
Fil: Gómez, Facundo A. Universidad de La Serena. Departamento de Física y Astronomía; Chile.
Fil: Cincotta, Pablo M. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Grupo de Caos en Sistemas Hamiltonianos; Argentina.
Fil: Giordano, Claudia M. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Grupo de Caos en Sistemas Hamiltonianos; Argentina.
Fil: Grand, Robert J. Heidelberger Institut fur Theoretische Studien; Alemania.
Fil: Marinacci, Federico. MIT. Kavli Institute for Astrophysics and Space Researc. Department of Physics; USA.
Fil: Pakmor, Rudiger. Heidelberger Institut fur Theoretische Studien; Alemania
Fil: Simpson, Christine M. Heidelberger Institut fur Theoretische Studien; Alemania
Fil: Springel, Volker. Max Planck Institut for Astrophysik; Alemania
Fil: Frenk, Carlos. Durham University. Institute for Computational Cosmology. Department of Physics; UK.
Fil: Maffione, Nicolás P. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Gómez, Facundo A. Universidad de La Serena. Instituto de Investigación Multidisciplinar en Ciencia y Tecnología; Chile
Fil: Gómez, Facundo A. Max Planck Institute for Astrophysics; Alemania
Fil: Cincotta, Pablo M. Universidad Nacional de La Plata. Instituto de Astrofísica de La Plata. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Giordano, Claudia M. Universidad Nacional de La Plata. Instituto de Astrofísica de La Plata. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Grand, Robert J. Zentrum fur Astronomie der Universitat Heidelberg. Astronomisches Rechen institut; Alemania
Fil: Springel, Volker. Heidelberger Institut fur Theoretische Studien; Alemania.
Fil: Springel, Volker. Zentrum fur Astronomie der Universitat Heidelberg. Astronomisches Rechen institut; Alemania
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.
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.