947 research outputs found
Multi-dimensional radiative transfer to analyze Hanle effect in Ca {\sc ii} K line at 3933 \AA\,
Radiative transfer (RT) studies of the linearly polarized spectrum of the Sun
(the second solar spectrum) have generally focused on the line formation, with
an aim to understand the vertical structure of the solar atmosphere using
one-dimensional (1D) model atmospheres. Modeling spatial structuring in the
observations of the linearly polarized line profiles requires the solution of
multi-dimensional (multi-D) polarized RT equation and a model solar atmosphere
obtained by magneto-hydrodynamical (MHD) simulations of the solar atmosphere.
Our aim in this paper is to analyze the chromospheric resonance line Ca {\sc
ii} K at 3933 \AA\ using multi-D polarized RT with Hanle effect and partial
frequency redistribution in line scattering. We use an atmosphere which is
constructed by a two-dimensional snapshot of the three-dimensional MHD
simulations of the solar photosphere, combined with columns of an 1D atmosphere
in the chromosphere. This paper represents the first application of polarized
multi-D RT to explore the chromospheric lines using multi-D MHD atmospheres,
with PRD as the line scattering mechanism. We find that the horizontal
inhomogeneities caused by MHD in the lower layers of the atmosphere are
responsible for strong spatial inhomogeneities in the wings of the linear
polarization profiles, while the use of horizontally homogeneous chromosphere
(FALC) produces spatially homogeneous linear polarization in the line core
Polarized Line Formation in Multi-Dimensional Media.III. Hanle Effect with Partial Frequency Redistribution
In the previous two papers, namely, \citet{anuknn11} and \citet{anuetal11} we
solved the polarized radiative transfer (RT) equation in multi-dimensional
(multi-D) geometries, with partial frequency redistribution (PRD) as the
scattering mechanism. We assumed Rayleigh scattering as the only source of
linear polarization () in both these papers. In this paper we extend
these previous works to include the effect of weak oriented magnetic fields
(Hanle effect) on line scattering. We generalize the technique of Stokes vector
decomposition in terms of the irreducible spherical tensors ,
developed in \citet{anuknn11}, to the case of RT with Hanle effect. A fast
iterative method of solution (based on the Stabilized Preconditioned
Bi-Conjugate-Gradient technique), developed in \citet{anuetal11}, is now
generalized to the case of RT in magnetized three-dimensional media. We use the
efficient short-characteristics formal solution method for multi-D media,
generalized appropriately to the present context. The main results of this
paper are the following: (1) A comparison of emergent profiles
formed in one-dimensional (1D) media, with the corresponding emergent,
spatially averaged profiles formed in multi-D media, shows that in the
spatially resolved structures, the assumption of 1D may lead to large errors in
linear polarization, especially in the line wings. (2) The multi-D RT in
semi-infinite non-magnetic media causes a strong spatial variation of the
emergent profiles, which is more pronounced in the line wings. (3)
The presence of a weak magnetic field modifies the spatial variation of the
emergent profiles in the line core, by producing significant
changes in their magnitudes.Comment: 31 pages, 14 figures, Submitted to ApJ, Under revie
Effect of cross-redistribution on the resonance scattering polarization of O {\sc i} line at 1302 \AA\,
Oxygen is the most abundant element on the Sun after Hydrogen and Helium. The
intensity spectrum of resonance lines of neutral Oxygen namely O {\sc i} (1302,
1305 and 1306 \AA\,) has been studied in the literature for chromospheric
diagnostics. In this paper we study the resonance scattering polarization in
the O {\sc i} line at 1302 \AA\, using two-dimensional radiative transfer in a
composite atmosphere constructed using a two-dimensional magneto-hydrodynamical
snapshot in the photosphere and columns of the one-dimensional FALC atmosphere
in the chromosphere. The methods developed by us recently in a series of papers
to solve multi-dimensional polarized radiative transfer have been incorporated
in our new code POLY2D which we use for our analysis. We find that
multi-dimensional radiative transfer including XRD effects is important in
reproducing the amplitude and shape of scattering polarization signals of the O
{\sc i} line at 1302 \AA\,
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