  A fully analytical formulation is developed to make dynamical friction
modeling more realistic. The rate for a satellite to decay its orbit in a host
galaxy halo is often severely overestimated when applying ChandraSekhar's
formula without correcting for the tidal loss of the satellite and the
adiabactic growth of the host galaxy potential over the Hubble time. As a
satellite decays to the inner and denser region of the host galaxy, the high
ambient density speeds up their exchange of energy and angular momentum, but
shrinks the Roche lobe of the satellite by tides. Eventually both processes of
orbital decay and tidal stripping hang up altogether once the satellite is
light enough. These competing processes can be modeled analytically for a
satellite if we parametrize the massloss history by an empirical formula. We
also incorporate the adiabatic contraction of orbits due to growth of the host
potential well. Observed dwarf galaxies often show a finite density core, which
determines how much inwards its remnants could be delivered to the host galaxy.
Ghost streams or remnant cores or globular clusters of satellites should
populate preferentially the outer halo (e.g., the Magellanic stream and the
Ursa Minor dwarf), rather than the inner halo (e.g., the Sgr stream and the
Omega-cen cluster). Massloss due to strong tides in the inner galaxy also makes
it problematic for any small central black holes in nuclei of satellite
galaxies to decay in orbit and merge into the center of the host galaxy.
