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EUV Line Intensities of Fe X

Published online by Cambridge University Press:  12 April 2016

P.R. Young ,
H.E. Mason ,
A.K. Bhatia ,
G.A. Doschek  and
R.J. Thomas
P.R. Young
Affiliation:
Department of Applied Mathematics and Theoretical Physics, Silver Street, Cambridge CB3 9EW, UK
H.E. Mason
Affiliation:
Department of Applied Mathematics and Theoretical Physics, Silver Street, Cambridge CB3 9EW, UK
A.K. Bhatia
Affiliation:
Laboratory for Astronomy and Solar Physics, Code 680, NASA-Goddard Space Flight Center, Greenbelt MD 20771, USA
G.A. Doschek
Affiliation:
E.O. Hulburt Center for Space Research, Naval Research Laboratory, Washington DC 20375-5000, USA
R.J. Thomas
Affiliation:
Laboratory for Astronomy and Solar Physics, Code 680, NASA-Goddard Space Flight Center, Greenbelt MD 20771, USA

Abstract

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The 4 configuration, distorted wave calculation of Bhatia & Doschek (1995) (hereafter referred to as BD95), together with the ground transition calculation of Pelan & Berrington (1995) are here used to predict the intensities of the Fe X EUV lines, which are then used to derive electron densities from several solar spectra, including the recent SERTS spectra.

Type
XIII. Plasma Diagnostics
Information
International Astronomical Union Colloquium , Volume 152: Astrophysics in the Extreme Ultraviolet , 1996 , pp. 583 - 587
Copyright
Copyright © Kluwer 1996

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