  The accreted component of stellar halos is composed of the contributions of
several satellites, falling onto their host with their different masses, at
different times, on different orbits. This work uses a suite of idealised,
collisionless N-body simulations of minor mergers and a particle tagging
technique to understand how these different ingredients shape each contribution
to the accreted halo, in both density and kinematics. I find that more massive
satellites deposit their stars deeper into the gravitational potential of the
host, with a clear segregation enforced by dynamical friction. Earlier
accretion events contribute more to the inner regions of the halo; more
concentrated subhaloes sink deeper through increased dynamical friction. The
orbital circularity of the progenitor at infall is only important for low-mass
satellites: dynamical friction efficiently radialises the most massive minor
mergers erasing the imprint of the infall orbit for satellite-to-host virial
mass ratios $\gtrsim1/20$. The kinematics of the stars contributed by each
satellite is also ordered with satellite mass: low-mass satellites contribute
fast-moving populations, in both ordered rotation and radial velocity
dispersion. In turn, contributions by massive satellites have lower velocity
dispersion and lose their angular momentum to dynamical friction, resulting in
a strong radial anisotropy.
