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A revisit to model the Cr i triplet at 5204-5208 Å and the Ba ii D2 line at 4554 Å in the Second Solar Spectrum

Published online by Cambridge University Press:  24 July 2015

H. N. Smitha
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore, India email: smithahn@iiap.res.in; knn@iiap.res.in; sampoorna@iiap.res.in
K. N. Nagendra
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore, India email: smithahn@iiap.res.in; knn@iiap.res.in; sampoorna@iiap.res.in
J. O. Stenflo
Affiliation:
Institute of Astronomy, ETH Zurich, CH-8093 Zurich, Switzerland email: stenflo@astro.phys.ethz.ch Istituto Ricerche Solari Locarno, Via Patocchi, 6605 Locarno-Monti, Switzerland email: mbianda@irsol.ch; ramelli@irsol.ch
M. Bianda
Affiliation:
Istituto Ricerche Solari Locarno, Via Patocchi, 6605 Locarno-Monti, Switzerland email: mbianda@irsol.ch; ramelli@irsol.ch
M. Sampoorna
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore, India email: smithahn@iiap.res.in; knn@iiap.res.in; sampoorna@iiap.res.in
R. Ramelli
Affiliation:
Istituto Ricerche Solari Locarno, Via Patocchi, 6605 Locarno-Monti, Switzerland email: mbianda@irsol.ch; ramelli@irsol.ch
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Abstract

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In our previous attempt to model the Stokes profiles of the Cr i triplet at 5204-5208 Å and the Ba ii D2 at 4554 Å, we found it necessary to slightly modify the standard FAL model atmospheres to fit the observed polarization profiles. In the case of Cr i triplet, this modification was done to reduce the theoretical continuum polarization, and in the case of Ba ii D2, it was needed to reproduce the central peak in Q/I. In this work, we revisit both these cases using different standard model atmospheres whose temperature structures closely resemble those of the modified FAL models, and explore the possibility of synthesizing the line profiles without the need for small modifications of the model atmosphere.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2015 

References

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A revisit to model the Cr i triplet at 5204-5208 Å and the Ba ii D2 line at 4554 Å in the Second Solar Spectrum
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A revisit to model the Cr i triplet at 5204-5208 Å and the Ba ii D2 line at 4554 Å in the Second Solar Spectrum
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A revisit to model the Cr i triplet at 5204-5208 Å and the Ba ii D2 line at 4554 Å in the Second Solar Spectrum
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