Abstract
Recent works showed that the absorbing material in broad absorption line (BAL) quasars is optically thick to major resonant absorption lines. This material may contribute significantly to the polarization in the absorption lines. In this paper, we present a detailed study of the resonant line scattering process using a Monte Carlo method to constrain the optical depth, the geometry, and the kinematics of the BAL region (BALR). By comparing our results with observed polarized spectra of BAL quasars, we find the following: (1) Resonant scattering can produce polarization up to 9% at the absorption trough for doublet transitions and up to 20% for singlet transitions in radially accelerated flows. To explain the large polarization degree in the C IV and N V absorption-line troughs detected in a small fraction of BAL QSOs, a nonmonotonic velocity distribution along the line of sight or/and additional contribution from the electron-scattering region is required. (2) The rotation of the flow can lead to the rotation of the polarization position angle (PA) in the line trough. A large extending angle of BALR is required to produce the observed large PA rotation in a few BAL QSOs. (3) A large extending angle of BALR is required to explain a subtrough in the polarized flux that was observed in a number of BAL QSOs. (4) The resonant scattering can contribute a significant part of N V emission line in some QSOs, and it may give rise to anomalous strong N V lines in these quasars. (5) The polarized flux and PA rotation produced by the resonant scattering regions is uniquely asymmetric, which may be used to test the presence of BALR in non-BAL QSOs.
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