  We track subhalo orbits of galaxy and group sized halos in cosmological
simulations. We identify filamentary structures around halos and we use these
to define a sample of subhalos accreted from filaments as well as a control
sample of subhalos accreted from other directions. We use these samples to
study differences in satellite orbits produced by filamentary accretion. Our
results depend on host halo mass. We find that for low masses, subhalos
accreted from filaments show $\sim10\%$ shorter lifetimes compared to the
control sample, they show a tendency towards more radial orbits, reach halo
central regions earlier, and are more likely to merge with the host. For higher
mass halos this lifetime difference dissipates and even reverses for cluster
sized halos. This behavior appears to be connected to the fact that more
massive hosts are connected to stronger filaments with higher velocity
coherence and density, with slightly more radial subhalo orbits. Because
subhalos tend to follow the coherent flow of the filament, it is possible that
such thick filaments are enough to shield the subhalo from the effect of
dynamical friction at least during their first infall. We also identify subhalo
pairs/clumps which merge with one another after accretion. They survive as a
clump for only a very short time, which is even shorter for higher subhalo
masses, suggesting that the Magellanic Clouds and other Local group satellite
associations, may have entered the MW virial radius very recently and probably
are in their first infall. Filaments boost the accretion of satellite
associations.

Cosmology and Nongalactic Astrophysics;Astrophysics of Galaxies