dc.contributor.author |
Smitha, H. N |
|
dc.contributor.author |
Nagendra, K. N |
|
dc.contributor.author |
Stenflo, J. O |
|
dc.contributor.author |
Bianda, M |
|
dc.contributor.author |
Sampoorna, M |
|
dc.contributor.author |
Ramelli, R |
|
dc.contributor.author |
Anusha, L. S |
|
dc.date.accessioned |
2012-05-01T13:04:26Z |
|
dc.date.available |
2012-05-01T13:04:26Z |
|
dc.date.issued |
2012-05 |
|
dc.identifier.citation |
Astronomy & Astrophysics, Vol. 541, A24 |
en |
dc.identifier.uri |
http://hdl.handle.net/2248/5766 |
|
dc.description.abstract |
The scattering polarization in the solar spectrum is traditionally modeled with each spectral line treated separately, but this is generally inadequate for multiplets where J-state interference plays a significant role. Through simultaneous observations of all the 3 lines of a Cr I triplet, combined with realistic radiative transfer modeling of the data, we show that it is necessary to include J-state interference consistently when modeling lines with partially interacting fine structure components. Polarized line formation theory that includes J-state interference effects together with partial frequency redistribution for a two-term atom is used to model the observations. Collisional frequency redistribution is also accounted for. We show that the resonance polarization in the Cr I triplet is strongly affected by the partial frequency redistribution effects in the line core and near wing peaks. The Cr I triplet is quite sensitive to the temperature structure of the photospheric layers. Our complete frequency redistribution calculations in semi-empirical models of the solar atmosphere cannot reproduce the observed near wing polarization or the cross-over of the Stokes Q/I line polarization about the continuum polarization level that is due to the J-state interference. When however partial frequency redistribution is included, a good fit to these features can be achieved. Further, to obtain a good fit to the far wings, a small temperature enhancement of the FALF model in the photospheric layers is necessary. |
en |
dc.language.iso |
en |
en |
dc.publisher |
EDP Sciences |
en |
dc.relation.uri |
http://dx.doi.org/10.1051/0004-6361/201118466 |
en |
dc.rights |
© ESO |
en |
dc.subject |
Line: profiles |
en |
dc.subject |
Line:polarization |
en |
dc.subject |
Line:scattering |
en |
dc.subject |
Methods: numerical |
en |
dc.subject |
Methods: radiative transfer |
en |
dc.subject |
Sun: atmosphere |
en |
dc.title |
J-state interference signatures in the second solar spectrum. Modeling the Cr I triplet at 5204-5208 |
en |
dc.type |
Article |
en |