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Coronal magnetic field measurements using forbidden emission lines

Published online by Cambridge University Press:  27 November 2018

A. Megha ,
M. Sampoorna ,
K. N. Nagendra  and
K. Sankarasubramanian
A. Megha
Affiliation:
Indian Institute of Astrophysics, Bengaluru, India; email: megha@iiap.res.in
M. Sampoorna
Affiliation:
Indian Institute of Astrophysics, Bengaluru, India; email: megha@iiap.res.in
K. N. Nagendra
Affiliation:
Indian Institute of Astrophysics, Bengaluru, India; email: megha@iiap.res.in
K. Sankarasubramanian
Affiliation:
Indian Institute of Astrophysics, Bengaluru, India; email: megha@iiap.res.in ISRO Satellite Centre, Bengaluru, India CESSI, IISER, Kolkata, India
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Abstract

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The polarization measurement of coronal forbidden emission lines is the most promising method of determining the direction of magnetic fields in the corona. A classical theory for the forbidden lines was presented in Megha et al. (2017) for the case of arbitrary strength magnetic fields. Here we apply that theoretical formalism to study the effect of density distributions, magnetic field configurations, and velocity fields on the Stokes profiles formed in corona. For illustrations we use the atomic parameters of the [Fe xiii] 10747 Å coronal forbidden line.

Keywords

Sun: corona - Sun: magnetic fields - line: profiles - polarization
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S340: Long-term Datasets for the Understanding of Solar and Stellar Magnetic Cycles , February 2018 , pp. 61 - 62
Copyright
Copyright © International Astronomical Union 2018 

References

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