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@ARTICLE{Machado:840318,
      author       = {Machado, R. E. G. and Manos, T.},
      title        = {{C}haotic motion and the evolution of morphological
                      components in a time-dependent model of a barred galaxy
                      within a dark matter halo},
      journal      = {Monthly notices of the Royal Astronomical Society},
      volume       = {458},
      number       = {4},
      issn         = {1365-2966},
      address      = {Oxford},
      publisher    = {Oxford Univ. Press},
      reportid     = {FZJ-2017-07860},
      pages        = {3578 - 3591},
      year         = {2016},
      abstract     = {Studies of dynamical stability (chaotic versus regular
                      motion) in galactic dynamics often rely on static analytical
                      models of the total gravitational potential. Potentials
                      based upon self-consistent N-body simulations offer more
                      realistic models, fully incorporating the time-dependent
                      nature of the systems. Here we aim at analysing the
                      fractions of chaotic motion within different morphological
                      components of the galaxy. We wish to investigate how the
                      presence of chaotic orbits evolves with time, and how their
                      spatial distribution is associated with morphological
                      features of the galaxy. We employ a time-dependent
                      analytical potential model that was derived from an N-body
                      simulation of a strongly barred galaxy. With this analytical
                      potential, we may follow the dynamical evolution of
                      ensembles of orbits. Using the Generalized Alignment Index
                      (GALI) chaos detection method, we study the fraction of
                      chaotic orbits, sampling the dynamics of both the stellar
                      disc and of the dark matter halo. Within the stellar disc,
                      the global trend is for chaotic motion to decrease in time,
                      specially in the region of the bar. We scrutinized the
                      different changes of regime during the evolution (orbits
                      that are permanently chaotic, permanently regular, those
                      that begin regular and end chaotic, and those that begin
                      chaotic and end regular), tracing the types of orbits back
                      to their common origins. Within the dark matter halo,
                      chaotic motion also decreases globally in time. The inner
                      halo (r < 5 kpc) is where most chaotic orbits are found and
                      it is the only region where chaotic orbits outnumber regular
                      orbits, in the early evolution.},
      cin          = {INM-7},
      ddc          = {520},
      cid          = {I:(DE-Juel1)INM-7-20090406},
      pnm          = {333 - Anti-infectives (POF3-333)},
      pid          = {G:(DE-HGF)POF3-333},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:000375799500015},
      doi          = {10.1093/mnras/stw572},
      url          = {https://juser.fz-juelich.de/record/840318},
}