  Discoveries of planet- and stellar remnant-hosting pulsars challenge our
understanding as the violent supernova explosion that forms the pulsar
presumably destabilizes the system. Type II supernova explosions lead to the
formation of eccentric bound systems, free-floating planets, neutron stars,
pulsars, and white dwarfs. Analytical and numerical studies of high mass-loss
rate systems based on perturbation theory so far have focused mainly on
planet-star systems. In this paper, we extend our understanding of the fate of
planet-star and binary systems by assuming a homologous envelope expansion
model using a plausible ejection velocity ($1000-10000\,\mathrm{km/s}$),
envelope- and neutron star masses. The investigation covers secondary masses of
1-10MJup for planetary, and 1-20MSun for stellar companions. We conduct and
analyze over 2.5 million simulations assuming different semi-major axes (2.23 -
100au), eccentricities (0-0.8), and true-anomalies (0-2pi) for the companion.
In a homologous expansion scenario, we confirm that the most probable outcome
of the explosion is the destabilization of the system, while the retention of a
bound system requires a highly eccentric primordial orbit. In general, a higher
ejecta velocity results in a lower eccentricity orbit independent of secondary
mass. The explanation of close-in pulsar planets requires exotic formation
scenarios, rather than survival through the type II supernova explosion model.
Post-explosion bound star systems gain a peculiar velocity (<100\,km/s), even
though the explosion model is symmetric. The applied numerical model allows us
to derive velocity components for dissociating systems. The peculiar velocities
of free-floating planets and stellar corpses are in the range of 10^-6-275km/s.
