  We consider a simple scenario for the accretion of matter onto a neutron star
in order to understand processes in the inner pulsar magnetosphere during the
transition stage between different accretion modes. A simple quasi-spherical
accretion process onto rotating, magnetized compact object is analyzed in order
to search for the radiative signatures which could appear during transition
between ejecting and accreting modes. It is argued that different accretion
modes can be present in a single neutron star along different magnetic field
lines for specific range of parameters characterising the pulsar (rotational
period, surface magnetic field strength) and the density of surrounding medium.
The radiation processes characteristic for the ejecting pulsar, i.e. curvature
and synchrotron radiation produced by primary electrons in the pulsar outer
gap, are expected to be modified by the presence of additional thermal
radiation from the neutron star surface. We predict that during the transition
from the pure ejector to the pure accretor mode (or vice versa) an intermediate
accretion state can be distinguished which is characterized by the $\gamma$-ray
spectra of pulsars truncated below ~1 GeV due to the absorption of
synchro-curvature spectrum produced in the pulsar gaps.
