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The Structure of the Prominence-Corona Interface

Published online by Cambridge University Press:  14 August 2015

F. Q. Orrall  and
R. J. Speer
F. Q. Orrall
Affiliation:
Institute for Astronomy, University of Hawaii, Honolulu, Hawaii, U.S.A.
R. J. Speer
Affiliation:
Dept. of Physics, Imperial College, London, England

Abstract

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The relatively cool Hα emitting regions of solar prominences are evidently surrounded by an interface or structure of intermediate temperature that separates them from the surrounding hot corona. At present, very little is known about this prominence-corona interface (hereafter called the PC interface), because most of its distinctive radiation is in the EUV where observations of high spatial resolution have not been available. In this paper we report on studies made on photometrically calibrated monochromatic images of prominences and the surrounding corona recorded on slitless spectra made during the eclipse of 1970, March 7. These were obtained with a rocket-borne Wadsworth spectrograph flown by the consortium group (Speer et al., 1970) and cover the range λλ850–2159 with a spectral resolution of 0.17 Å and a spatial resolution better than 10″ over half the spectrum. They include spectral lines of a number of ionic species from Hi through Nixv. Because each species exists in a rather narrow temperature range, some of the monochromatic images show the low temperature prominence itself; some the coronal structure surrounding it; and some the intermediate structure we have called the PC interface.

Type
Part V: The Chromosphere in Active Regions
Information
Symposium - International Astronomical Union , Volume 56: Chromospheric Fine Structure , 1974 , pp. 193 - 196
Copyright
Copyright © Reidel 1974 

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