Warm Absorbers in X-rays (WAX), a comprehensive high resolution grating
  spectral study of a sample of Seyfert Galaxies: II. Warm Absorber dynamics
  and feedback to galaxies
  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 ($15-17\rm \AA$) have more mass outflow rates.
