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A Model for the North Coronal Hole Observed at the 1973 Eclipse, Between 1.3 and 3.2 R⊙

Published online by Cambridge University Press:  14 August 2015

Francoise Crifo  and
Jean-Pierre Picat
Francoise Crifo
Affiliation:
D.A.P.H.E. - Observatoire de Meudon 92 190 - Meudon, France
Jean-Pierre Picat
Affiliation:
D.A.P.H.E. - Observatoire de Meudon 92 190 - Meudon, France

Extract

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At the 1973 eclipse, S. Koutchmy (Institut d'Astrophysique, Paris) obtained several pictures of the white-light corona, using polarizers and a radially-compensated filter. These pictures provide a very good opportunity for studying the large coronal hole at the north polar cap; this hole has been extensively studied during the Skylab period. On the plates of Koutchmy, we could record reliable intensities between 1.3 and 3.2 R⊙. The absolute calibration was made using the stars observed in the field at the same time. This method allows a direct comparison of well-exposed objects on a same plate and must therefore be highly reliable (see Koutchmy et al., 1978). It is well-known that the absolute calibration of eclipse plates is a difficult problem.

Type
Part I. The Life History of Coronal Structures and Fields
Information
Symposium - International Astronomical Union , Volume 91: Solar and Interplanetary Dynamics , 1980 , pp. 45 - 48
Copyright
Copyright © Reidel 1980 

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