Long-Term Variation of Solar Coronal Fe XIV and Fe X Fluxes

Details Long-Term Variation of Solar Coronal Fe XIV and Fe X Fluxes Long-Term Variation of Solar Coronal Fe XIV and Fe X Fluxes

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.8809a&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #88.09; Bulletin of the American Astronomical Society, Vol. 34, p.790

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Scientific paper

Synoptic photoelectric observations of the coronal Fe XIV and Fe X emission lines at 530.3 nm and 637.4 nm, respectively, are analyzed to study the output of the solar corona in these lines as a function of time. The data used are measurements made with the NSO/Sacramento Peak 40-cm coronagraph and Emission-Line Coronal Photometer of the intensity of these lines observed at 1.15 solar radii between 1973 (1984 for Fe X) and 2002. A new calibration determination is used to convert relative intensities to absolute intensities. The solar-cycle variation of these fluxes will be compared to each other and to other solar-cycle parameters. One interesting result is that a constant minimum or basal corona may exist at solar minimum. This paper was supported by the Air Force Office of Scientific Research.

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