HAL Id: jpa-00227584
https://hal.archives-ouvertes.fr/jpa-00227584
Submitted on 1 Jan 1988
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THE INTERPRETATION OF SOLAR SPECTRAL INTENSITIES
R. Mcwhirter
To cite this version:
R. Mcwhirter. THE INTERPRETATION OF SOLAR SPECTRAL INTENSITIES. Journal de
Physique Colloques, 1988, 49 (C1), pp.C1-329-C1-329. �10.1051/jphyscol:1988170�. �jpa-00227584�
JOURNAL DE PHYSIQUE
Colloque Cl, Supplbment au n"3, Tome 49, Mars 1988
THE INTERPRETATION OF SOLAR SPECTRAL INTENSITIES
R.W.P. McWHIRTER
Rutherford Appleton Laboratory, Chflton, GB-Didcot OX11 OQX.
Great-Britain
The intensity of a specrtal line from an optically thin plasma such as the outer atmosphere of the sun depends on both the atomic properties of the atomic ion responsible for the line and the physical nature of t h e plasma. In this paper we discuss t h e various ways in which the measured spectral intensities from the sun are used t o discover something about tbe nature of the sun's atmosphere. The technique has been referred to as the emission measure method. It
has important limitations in terms of the accuracy of the specrtal d a t a as well as the atoniic data. We discuss some of these and suggest methods by which they may be assessed. The technique is illustrated by application t o real observations from a number of authors.
Article published online by EDP Sciences and available at http://dx.doi.org/10.1051/jphyscol:1988170
