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We present both phenomenological and more physical photoionization models ofthe Chandra HETG spectra of the Seyfert-1 AGN NGC 4051. We detect 40 absorptionand emission lines, encompassing highly ionized charge states from O, Ne, Mg,Si, S and the Fe L-shell and K-shell. Two independent photoionization packages,XSTAR and Cloudy, were both used to self-consistently model the continuum andline spectra. These fits detected three absorbing regions in this system withdensities ranging from 10^{10} to 10^{11} cm^{-3}. In particular, our XSTARmodels require three components that have ionization parameters of log \xi =4.5, 3.3, & 1.0, and are located within the BLR at 70, 300, and 13,000 R_g,respectively, assuming a constant wind density. Larger radii are inferred fordensity profiles which decline with radius. The Cloudy models give a similarset of parameters with ionization parameters of log \xi = 5.0, 3.6, & 2.2located at 40, 200, and 3,300 R_g. We demonstrate that these regions areout-flowing from the system, and carry a small fraction of material out of thesystem relative to the implied mass accretion rate. The data suggest thatmagnetic fields may be an important driving mechanism.

Warm Absorbers and Outflows in the Seyfert-1 Galaxy NGC 4051