  Since the discovery of exoplanets around pulsars, there has been a debate on
their origin. Popular scenarios include in situ formation or the dynamical
capture of a planet in a dense stellar system. The possibility of a planet
surviving its host star's supernova is often neglected, because a planet in
orbit around a single exploding star is not expected to survive the supernova.
A circum-binary planet, however, may stand a chance in staying bound when one
of the binary components explodes. We investigate the latter and constrain the
distribution of post-supernova orbital parameters of circum-binary planets.
This is done by performing population synthesis calculations of binary stars
until the first supernova. Just before the supernova, we add a planet in orbit
around the binary to study its survivability. In our supernova model, the
exploding star's mass is assumed to change instantaneously, and we apply a
velocity kick to the newly formed remnant. The mass loss and velocity kick
affect the orbits of the two stars and the planet. Only $2 \cdot 10^{-3}$ of
systems survive the supernova while keeping the circum-binary planet bound. The
surviving planetary orbits are wide ($a \apgt 10$ au) and eccentric ($e \apgt
0.3$). It turns out much more likely ($3\cdot 10^{-2}$ system fraction) that
the newly formed compact object is ejected from the system, leaving the planet
bound to its companion star in a highly eccentric orbit (typically $\apgt
0.9$). We expect that the Milky way Galaxy hosts at most $10$ x-ray binaries
that are still orbited by a planet, and $\aplt 150$ planets that survived in
orbit around the compact object's companion. These numbers should be convolved
with the fraction of massive binaries that is orbited by a planet.
