Spectral Signatures of Winds from Accretion Disks around Black Holes

Accretion and outflows are common in systems which include compact objects such as black holes and neutron stars. In the last three decades, numerous models have been built to produce jets and outflows. In the case of black holes, since no matter can escape out of the horizon, some suggested that the jets are formed in the strong field region around black holes in the form of pair plasma (Type A) while others suggested that the jets come from the accretion disks (Type B). Models of Type A are still incomplete and most likely to be incorrect since jets are very generic, and equally energetic jets are also possible for neutron stars as well. Until 1998, all the Type B models envisaged that the whole accretion disk participates in the jet formation. In 1998, Chakrabarti suggested that because the centrifugal barrier dominated boundary layer (CENBOL) in an accretion flow is hot (being the post-shock region), it is more likely that jets would be produced from this region (Chakrabarti, 1998; 1999a). Outflow rate in units of inflow rate was also computed