  We have explored the dynamical and mass evolution of halos driven by
large-scale filaments using a dark matter-only cosmological simulation with the
help of a phase-space analysis. Since a non-negligible number of galaxies is
expected to fall into the cluster environment through large-scale filaments,
tracking how halos move around large-scale filaments can provide a more
comprehensive view on the evolution of cluster galaxies. Halos exhibit orbital
motions around filaments, which emerge as specific trajectories in a phase
space composed of halos' perpendicular distance and velocity component with
respect to filaments. These phase-space trajectories can be represented by
three cases according to their current states. We parameterize the trajectories
with halos' initial position and velocity, maximum velocity, formation time,
and time since first crossing, which are found to be correlated with each
other. These correlations are explained well in the context of the large-scale
structure formation. The mass evolution and dynamical properties of halos seem
to be affected by the density of filaments, which can be shown from the fact
that halos around denser filaments are more likely to lose their mass and be
bound within large-scale filaments. Finally we reproduce the mass segregation
trend around filaments found in observations. It is resulted because halos that
formed earlier arrived filaments earlier, and grew efficiently there being more
massive. We also found that dynamical friction helps to retain this segregation
trend.
