Spectral line polarization with angle-dependent partial frequency redistribution III. Single scattering approximation for the Hanle effect

@article{Sampoorna2011SpectralLP,
  title={Spectral line polarization with angle-dependent partial frequency redistribution III. Single scattering approximation for the Hanle effect},
  author={M. Sampoorna},
  journal={Astronomy and Astrophysics},
  year={2011},
  volume={532}
}
  • M. Sampoorna
  • Published 1 August 2011
  • Physics
  • Astronomy and Astrophysics
Context. The solar limb observations in spectral lines display evidence of linear polarization, caused by non-magnetic resonance scattering process. This polarization is modified by weak magnetic fields ‐ the process of the Hanle effect. These two processes serve as diagnostic tools for weak solar magnetic field determination. In modeling the polarimetric observations the partial frequency redistribution (PRD) effects in line scattering have to be accounted for. For simplicity, it is common… 
Spectral line polarization with angle-dependent partial frequency redistribution - IV. Scattering expansion method for the Hanle effect
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The spectral line polarization encodes a wealth of information about the thermal and magnetic properties of the solar atmosphere. Modeling the Stokes profiles of strong resonance lines is, however, a
POLARIZED LINE FORMATION IN MULTI-DIMENSIONAL MEDIA. IV. A FOURIER DECOMPOSITION TECHNIQUE TO FORMULATE THE TRANSFER EQUATION WITH ANGLE-DEPENDENT PARTIAL FREQUENCY REDISTRIBUTION
To explain the linear polarization observed in spatially resolved structures in the solar atmosphere, the solution of polarized radiative transfer (RT) equation in multi-dimensional (multi-D)

References

SHOWING 1-10 OF 13 REFERENCES
Spectral line polarization with angle-dependent partial frequency redistribution II Accelerated lambda iteration and scattering expansion methods for the Rayleigh scattering
Context. The linear polarization of strong resonance lines observed in the solar spectrum is created by the scattering of the photospheric radiation field. This polarization is sensitive to the form
Spectral line polarization with angle-dependent partial frequency redistribution - I. A Stokes parameters decomposition for Rayleigh scattering
Context. The linear polarization of a strong resonance lines observed near the solar limb is created by a multiple-scattering process. Partial frequency redistribution (PRD) effects must be accounted
Scattering of polarized light in spectral lines with partial frequency redistribution: general redistribution matrix
The redistribution matrix for resonance scattering of arbitrarily polarized light, described by a vector of Stokes parameters, is derived assuming that the ground state is isotropic (i.e., assuming
Hanle effect with angle-dependent partial redistribution
The polarized line transfer equation for the Hanle effect is solved in the framework of an exact partial frequency redistribution (PRD) theory developed by Bommier (1997a,b). In that theory the
GENERALIZATION OF THE LAST SCATTERING APPROXIMATION FOR THE SECOND SOLAR SPECTRUM MODELING: THE Ca I 4227 Å LINE AS A CASE STUDY
To model the second solar spectrum (the linearly polarized spectrum of the Sun that is due to coherent scattering processes), one needs to solve the polarized radiative transfer (RT) equation. For
The Hanle effect in a random magnetic field - Dependence of the polarization on statistical properties of the magnetic field
Context. The Hanle effect is used to determine weak turbulent magnetic fields in the solar atmosphere, usually assuming that the angular distribution is isotropic, the magnetic field strength
An operator perturbation method for polarized line transfer VI. Generalized PALI method for Hanle effect with partial frequency redistribution and collisions
A generalized iteration method is presented to solve the polarized line transfer equation for a two-level-atom in an arbitrarily oriented, weak magnetic field. The polarized redistribution matrix
The Hanle effect Decomposition of the Stokes parameters into irreducible components
Context. It has been shown for the weak-field Hanle effect that the Stokes parameters  I , Q , and U can be represented by a set of six cylindrically symmetrical functions. The proof relies on
The Hanle effect and the diagnostics of turbulent magnetic fields in the solar atmosphere
The theory of the Hanle effect is used to interpret the linear polarization measured in a number of spectral lines on the solar disk near the heliographic north and south poles, in search for a
Non-Coherent Scattering: I. The Redistribution Function with Doppler Broadening
The redistribution in frequency of radiation scattered from moving atoms is examined in some generality, allowing for the different types of scattering that occur in the atom's rest frame under
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