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Eclipse Polarimetric Research of Prominences

Published online by Cambridge University Press:  12 April 2016

A.N. Lebedev ,
I.A. Belenko ,
O.I. Bougaenko ,
I.S. Kim ,
O.T. Matsuura ,
E. Picazzio ,
R.P. Livi  and
Silvia H.B. Liv
A.N. Lebedev
Affiliation:
Sternberg State Astronomical Institute, Moscow State University Universitetsky pr. 13, 119899 Moscow, Russia
I.A. Belenko
Affiliation:
Sternberg State Astronomical Institute, Moscow State University Universitetsky pr. 13, 119899 Moscow, Russia
O.I. Bougaenko
Affiliation:
Sternberg State Astronomical Institute, Moscow State University Universitetsky pr. 13, 119899 Moscow, Russia
I.S. Kim
Affiliation:
Sternberg State Astronomical Institute, Moscow State University Universitetsky pr. 13, 119899 Moscow, Russia
O.T. Matsuura
Affiliation:
Instituto Astronomico e Geofisico Universidade de São Paulo, Av. Miguel Stefano, 4200 CEP 04301–904, São Paulo, SP, Brasil
E. Picazzio
Affiliation:
Instituto Astronomico e Geofisico Universidade de São Paulo, Av. Miguel Stefano, 4200 CEP 04301–904, São Paulo, SP, Brasil
R.P. Livi
Affiliation:
Instituto de Fisica UFRGS, Campus do Vale, Av. Bento Goncalves, 9500 CEP 91501–970, Porto Alegre–RS, Brasil
Silvia H.B. Liv
Affiliation:
Instituto de Fisica UFRGS, Campus do Vale, Av. Bento Goncalves, 9500 CEP 91501–970, Porto Alegre–RS, Brasil

Abstract

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A polarization analysis of E–limb prominences on November 3, 1994 is presented. Photometry and data reduction of 24 prominence pictures based on IDL software and Stokes–vector presentation and applied to Hα emission resulted in an accuracy of 1–1.5% in determination of the polarization degree and of 1.5–2.0° in the polarization direction. Distributions of polarization degree (polarization images) for prominences and the “white light” corona are presented. A polarization degree of 2–5% for prominences and 10–25% for the nearby white light corona are found. The polarization direction is found to be tangential to the solar limb. It is noted that eclipse observations can provide a powerful method for deriving the magnetic field at high altitudes in the coronal volume.

Type
Filaments and Their Environment
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 66 - 69
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

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