  The migration strength and direction of embedded low-mass planets depends on
the disc structure. In discs with an efficient radiative transport, the
migration can be directed outwards for planets with more than 3-5 Earth masses.
This is due to the entropy driven corotation torque, a process that extends the
lifetimes of growing planetary embryos. We investigate the influence on the
disc structure caused by a jump in the alpha parameter of the viscosity to
model a dead-zone structure in the disc. We focus on M-dot discs, which have a
constant net mass flux. Using the resulting disc structure, we investigate the
consequences for the formation of planetesimals and determine the regions of
outward migration for proto-planets. We performed numerical hydrosimulations of
M-dot discs in the r-z-plane. We used the explicit/implicit hydrodynamical code
FARGOCA that includes a full tensor viscosity and stellar irradiation as well
as a two-temperature solver that includes radiation transport in the
flux-limited diffusion approximation. Viscosity transitions inside the disc
create transitions in density that stop inward migration for small planets
through the so-called "planet trap" mechanism. This mechanism also works for
planets down to M_P > 0.5M_E. Additionally, the viscosity transitions change
the pressure gradient in the disc, which facilitates planetesimal formation via
the streaming instability. However, a very steep transition in viscosity is
needed to achieve in a pressure bump in the disc. The transition in viscosity
facilitates planetesimal formation and can stop the migration of small-mass
planets (M_P>0.5M_E), but still does not halt inward migration of smaller
planets and planetesimals that are affected by gas drag. A very steep, probably
unrealistic viscosity gradient is needed to trap planets of smaller masses and
halt gas-drag-driven planetesimal migration at a pressure bump.
