Abstract:
We investigate the role of radiative driving of shock-ejected bipolar outflows from advective
accretion discs in a self-consistent manner. Radiations from the inner disc affects the subsonic
part of the jet while those from the pre-shock disc affects the supersonic part, and there by
constitutes a multistage acceleration process. We show that the radiation from the inner disc
not only accelerate but also increase the mass outflow rate, while the radiation from the preshock
disc only increases the kinetic energy of the flow. With proper proportions of these two
radiations, very high terminal speed is possible. We also estimated the post-shock luminosity
from the pre-shock radiations, and showed that with the increase of viscosity parameter the disc
becomes more luminous, and the resulting jet simultaneously becomes faster. This mimics the
production of steady mildly relativistic but stronger jets as microquasars move from low-hard
to intermediate-hard spectral states.
