The impact of quantum interferences between different J-levels on scattering polarization in spectral lines

Abstract

The spectral line polarization produced by optically pumped atoms contains a wealth of information on the thermal and magnetic structure of a variety of astrophysical plasmas, including that of the solar atmosphere. A correct decoding of such information from the observed Stokes profiles requires a clear understanding of the effects that radiatively induced quantum interferences (or coherences) between pairs of magnetic sublevels produce on these observables, in the absence and in the presence of magnetic fields of arbitrary strength. Here we present a detailed theoretical investigation on the role of coherences between pairs of sublevels pertaining to different fine-structure J-levels, clarifying when they can be neglected for facilitating the modeling of the linear polarization produced by scattering processes in spectral lines. To this end, we apply the quantum theory of spectral line polarization and calculate the linear polarization patterns of the radiation scattered at 90 degrees by a slab of stellar atmospheric plasma, taking into account and neglecting the above-mentioned quantum interferences. Particular attention is given to the 2S-2P, 5S-5P, and 3P-3S multiplets. We point out the observational signatures of this kind of interferences and analyze their sensitivity to the energy separation between the interfering levels, to the amount of emissivity in the background continuum radiation, to lower-level polarization, and to the presence of a magnetic field. Some interesting applications to the following spectral lines are also presented: CaII H and K, MgII h and k, NaI D1 and D2, the BaII 4554A and 4934A resonance lines, the CrI triplet at 5207A, the OI triplet at 7773A, the MgI b-lines, and the H-alpha and Ly-alpha lines of HI.

Accepted for publication in The Astrophysical Journal

References in corpus (2)

• The Magnetic Sensitivity of the Ba II D1 and D2 Lines of the Fraunhofer Spectrum
• Scattering Polarization of Hydrogen Lines in Weakly Magnetized Stellar Atmospheres I. Formulation and Application to Isothermal Models

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