We examine the orbits of satellite galaxies identified in a suite of N-body/gasdynamical simulations of the formation of L ∗ galaxies in a ΛCDM universe. The numerical resolution of the simulations allows us to track in detail the orbits of the ∼ ten brightest satellites around each primary. Most satellites follow conventional orbits; after turning around, they accrete into their host halo and settle on orbits whose apocentric radii are steadily eroded by dynamical friction. As a result, satellites associated with the primary are typically found within its virial radius, rvir, and have velocities consistent with a Gaussian distribution with mild radial anisotropy. However, a number of outliers are also present. We find that a surprising number (about one-third) of satellites identified at z = 0 are on unorthodox orbits, with apocenters that exceed their turnaround radii. These include a number of objects with extreme velocities and apocentric radii at times exceeding ∼ 3.5 rvir (or, e.g., ∼> 1 Mpc when scaled to the Milky Way). This population of satellites on extreme orbits consists typically of the faint member of a satellite pair whose kinship is severed by the tidal field of the primary during first approach. Under the right circumstances, the heavier member of the pair remains bound to th
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