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Polarized Line Formation in Arbitrary Strength Magnetic Fields Angle-averaged and Angle-dependent Partial Frequency Redistribution

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dc.contributor.author Sampoorna, M
dc.contributor.author Nagendra, K. N
dc.contributor.author Stenflo, J. O
dc.date.accessioned 2020-11-11T01:08:08Z
dc.date.available 2020-11-11T01:08:08Z
dc.date.issued 2017-08
dc.identifier.citation The Astrophysical Journal, Vol. 844, No. 2, 97 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6818
dc.description Restricted Access © The American Astronomical Society https://doi.org/10.3847/1538-4357/aa7a15 en_US
dc.description.abstract Magnetic fields in the solar atmosphere leave their fingerprints in the polarized spectrum of the Sun via the Hanle and Zeeman effects. While the Hanle and Zeeman effects dominate, respectively, in the weak and strong field regimes, both these effects jointly operate in the intermediate field strength regime. Therefore, it is necessary to solve the polarized line transfer equation, including the combined influence of Hanle and Zeeman effects. Furthermore, it is required to take into account the effects of partial frequency redistribution (PRD) in scattering when dealing with strong chromospheric lines with broad damping wings. In this paper, we present a numerical method to solve the problem of polarized PRD line formation in magnetic fields of arbitrary strength and orientation. This numerical method is based on the concept of operator perturbation. For our studies, we consider a two-level atom model without hyperfine structure and lower-level polarization. We compare the PRD idealization of angle-averaged Hanle–Zeeman redistribution matrices with the full treatment of angle-dependent PRD, to indicate when the idealized treatment is inadequate and what kind of polarization effects are specific to angledependent PRD. Because the angle-dependent treatment is presently computationally prohibitive when applied to realistic model atmospheres, we present the computed emergent Stokes profiles for a range of magnetic fields, with the assumption of an isothermal one-dimensional medium. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Line: profiles en_US
dc.subject Polarization en_US
dc.subject Radiative transfer en_US
dc.subject Scattering en_US
dc.subject Sun: atmosphere en_US
dc.title Polarized Line Formation in Arbitrary Strength Magnetic Fields Angle-averaged and Angle-dependent Partial Frequency Redistribution en_US
dc.type Article en_US


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