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Using Strong Solar Coronal Emission Lines as Coronal Flux ProxiesA comparison of Skylab results with observations of the strong EUV lines of Fe XVI at 335 A and 361 A from the Goddard Solar EUV Rocket Telescope and Spectrograph (SERTS) flight of 1989 suggests that these lines, and perhaps others observed with SERTS, might offer good proxies for estimating the total coronal flux over important wavelength ranges. In this paper, we compare SERTS observations from a later, 1993 flight with simultaneous cospatial Yohkoh soft X-ray observations to test this suggestion over the energy range of the Soft X-ray Telescope (SXT) on Yohkoh. Both polynomial and power-law fits are obtained, and errors are estimated, for the SERTS lines of Fe XVI 335 A and 361 A, Fe XV 284 A and 417 A, and Mg IX 368 A. It is found that the power-law fits best cover the full range of solar conditions from quiet Sun through active region, though not surprisingly the 'cooler' Mg IX 368 A line proves to be a poor proxy. The quadratic polynomial fits yield fair agreement over a large range for all but the Mg IX line, but the linear fits fail conspicuously when extrapolated into the quiet Sun regime. The implications of this work for the He 11 304 A line formation problem are briefly considered. The paper concludes with a discussion of the value of these iron lines observed with SERTS for estimating stellar coronal fluxes, as observed for example with the EUVE satellite.
Document ID
19990105828
Acquisition Source
Marshall Space Flight Center
Document Type
Reprint (Version printed in journal)
Authors
Falconer, David A.
(NASA Marshall Space Flight Center Huntsville, AL United States)
Jordan, Studart D.
(NASA Goddard Space Flight Center Greenbelt, MD United States)
Davila, Joseph M.
(NASA Goddard Space Flight Center Greenbelt, MD United States)
Thomas, Roger J.
(NASA Goddard Space Flight Center Greenbelt, MD United States)
Andretta, Vincenzo
(NASA Goddard Space Flight Center Greenbelt, MD United States)
Brosius, Jeffrey W.
(Hughes STX United States)
Hara, Hirosha
(National Astronomical Observatory Tokyo, Japan)
Date Acquired
August 19, 2013
Publication Date
January 1, 1997
Subject Category
Solar Physics
Distribution Limits
Public
Copyright
Other

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