MAGNETICALLY DRIVEN ACCRETION DISK WINDS AND ULTRA-FAST OUTFLOWS IN PG 1211+143

We present a study of X-ray ionization of MHD accretion-disk winds in an effort to constrain the physics underlying the highly ionized ultra-fast outflows (UFOs) inferred by X-ray absorbers often detected in various sub. classes of Seyfert active galactic nuclei (AGNs). Our primary focus is to show that magnetically driven outflows are indeed physically plausible candidates for the observed outflows accounting for the AGN absorption properties of the present X-ray spectroscopic observations. Employing a stratified MHD wind launched across the entire AGN accretion disk, we calculate its X-ray ionization and the ensuing X-ray absorption-line spectra. Assuming an appropriate ionizing AGN spectrum, we apply our MHD winds to model the absorption features in an XMM-Newton/EPIC spectrum of the narrow-line Seyfert, PG 1211+143. We find, through identifying the detected features with Fe K alpha transitions, that the absorber has a characteristic ionization parameter of log (xi(c)[erg cm s(-1)]) similar or equal to 5-6 and a column density on the order of N-H similar or equal to 10(23) cm(-2) outflowing at a characteristic velocity of v(c)/c similar or equal to 0.1-0.2 (where c is the speed of light). The best-fit model favors its radial location at r(c) similar or equal to 200 R-o (R-o is the black hole's innermost stable circular orbit), with an inner wind truncation radius at R-t similar or equal to 30 R-o. The overall K-shell feature in the data is suggested to be dominated by Fe XXV with very little contribution from Fe XXVI and weakly ionized iron, which is in good agreement with a series of earlier analyses of the UFOs in various AGNs, including PG 1211+143.