Planet formation can occur in radiation-driven low-mass
X-ray binaries (RD-LMXBs) with evolutionary timescales
[25] whose mass-loss rates are enhanced
by X-ray irradiation [5,6,13,21] and that turn at a later stage
into SVPs [5]. Again a circum-binary disk can form at large
distance if a substantial fraction of the mass outflow is
gravitationally bound. The mass-loss rates involved in this case are
, and a small fraction of
the mass loss of order 
needs to be trapped in the system
depending on the chemical composition of the outflowing material. We
ran several two-dimensional and preliminary three-dimensional SPH
models of LMXB outflows (whose results are to be reported elsewhere;
manuscript in preparation) and obtained the necessary f for a
variety of orbital parameters, 
and 
. In
this case, planet formation can proceed in a way similar to the
mechanism suggested in [19], with the crucial difference of
having much more angular momentum available. Only at distances
from the central power source (now an X-ray
source possibly screened by the accretion disk material) can the
outflow material cool down to temperatures that allow grain and
planetesimal formation. The irradiation-driven mass loss of RD-LMXBs
is expected to be suddenly quenched after 
[6,21,25], and such systems can result in binaries consisting of
spun-up millisecond pulsars with low-mass companions[5]. The
binary then turns into an SVP if the pulsar is sufficiently powerful
and the companion is relatively close, and the evolution described
above can be applied for the later stages of binary evolution. We note
that the planets formed during a previous RD-LMXB phase can survive
the second SVP phase.