Temporal characteristics of the solar UV flux and He I line at 1083 NM

Details Temporal characteristics of the solar UV flux and He I line at 1083 NM Temporal characteristics of the solar UV flux and He I line at 1083 NM

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985jgr....90.6267d&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 90, July 1, 1985, p. 6267-6273. NOAA-NASA-supported research.

Astronomy and Astrophysics

Astronomy

40

Helium, Infrared Spectra, Solar Flux, Solar Spectra, Ultraviolet Astronomy, Amplitude Distribution Analysis, Atmospheric Effects, Power Spectra, Solar Rotation, Temporal Distribution

Scientific paper

It is pointed out that the solar UV flux in the 170- to 210-nm range is important because it photodissociates O2 in the terrestrial atmosphere and thereby initiates the production of ozone and other odd-oxygen chemistry in the stratosphere. The 210- to 290-nm solar UV flux heats the stratosphere. There is consequently a great interest in the temporal variations of the solar UV flux and its relation to ground-based measures of solar activity which may be useful in estimating the UV flux variations. The present investigation is concerned with daily values of 205-nm solar UV flux data measured with the aid of the Nimbus 7 satellite during the period from November 1978 to November 1982, taking into account also measurements of the equivalent width of the He I solar absorption line at 1083 at the National Solar Observatory. Attention is given to an analysis of the data, episodes of activity, and long-term variations.

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