Temporal variations of solar UV spectral irradiance caused by solar rotation and active region evolution

Details Temporal variations of solar UV spectral irradiance caused by solar rotation and active region evolution Temporal variations of solar UV spectral irradiance caused by solar rotation and active region evolution

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984siva.work..233d&link_type=abstract

In NASA, Washington Solar Irradiance Variations on Active Region Time Scales p 233-252 (SEE N84-27635 17-92)

Computer Science

1

Irradiance, Periodic Variations, Solar Activity, Solar Rotation, Ultraviolet Radiation, Atmospheric Chemistry, Faculae, Solar Magnetic Field, Solar Terrestrial Interactions, Sunspots

Scientific paper

Variations in the solar 100 to 400 nm UV spectral irradiance caused by solar rotation and active region evolution, are discussed as a function of UV wavelength, CMD dependence, and in relation to the temporal variations in the total solar irradiance, 10.7 cm radio flux, sunspot number and Ca K plage data. Active region radiation at cm wavelengths includes a component proportional to the magnetic field. Active region evolution involves a more rapid growth, peak and decay of sunspots and their strong magnetic fields than the Ca K plages and their related UV enhancements. Major plages often last a rotation or more longer than the active region's sunspots. Large active regions, including those associated with major dips in the total solar irradiance, tend to produce the strongest peaks in 10.7 cm and sunspot numbers on their first rotation, while the Ca K plages and UV enhancements peak on the next rotation and decay more slowly on subsequent rotations. Differences in CMD dependencies cause temporal differences including the stronger presence of 13 day variations in the UV flux.

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