This paper is a sequel to the extensive study of warm absorber ( WA ) in X-rays carried out using high resolution grating spectral data from XMM-Newton satellite ( WAX-I ) .
Here we discuss the global dynamical properties as well as the energetics of the WA components detected in the WAX sample .
The slope of WA density profile ( n \propto r ^ { - \alpha } ) estimated from the linear regression slope of ionization parameter \xi and column density N _ { H } in the WAX sample is \alpha = 1.236 \pm 0.034 .
We find that the WA clouds possibly originate as a result of photo-ionised evaporation from the inner edge of the torus ( torus wind ) .
They can also originate in the cooling front of the shock generated by faster accretion disk outflows , the ultra-fast outflows ( UFO ) , impinging onto the interstellar medium or the torus .
The acceleration mechanism for the WA is complex and neither radiatively driven wind nor MHD driven wind scenario alone can describe the outflow acceleration .
However , we find that radiative forces play a significant role in accelerating the WA through the soft X-ray absorption lines , and also with dust opacity .
Given the large uncertainties in the distance and volume filling factor estimates of the WA , we conclude that the kinetic luminosity \dot { E } _ { K } of WA may sometimes be large enough to yield significant feedback to the host galaxy .
We find that the lowest ionisation states carry the maximum mass outflow , and the sources with higher Fe M UTA absorption ( 15 - 17 \AA ) have more mass outflow rates .