Rocket Observation of X-Ray Emission in a Solar Flare

Details Rocket Observation of X-Ray Emission in a Solar Flare Rocket Observation of X-Ray Emission in a Solar Flare

Apr 1957

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1957natur.179..861c&link_type=abstract

Nature, Volume 179, Issue 4565, pp. 861-862 (1957).

Physics

4

Scientific paper

FROM a dozen rocket flights scattered over the past seven years, we have obtained measurements of solar X-rays and far ultra-violet light that ionize the atmosphere above 70 km.1. These experiments revealed the emissions of a `quiet' sun, since none of the flights chanced to coincide with a solar flare. Briefly summarized, the results showed that the sun normally radiates sufficient X-ray energy between 10 A. and 100 A. to account for the E-region (100-140 km.). When coronal green- and red-line activity was high, X-ray intensities were observed to be correspondingly high and included wave-lengths shorter than 10 A. In the ultra-violet, the most prominent emission line observed in the solar spectrum was the Lyman α-line of hydrogen at 1216 A. This one emission line accounted for normal D-region ionization between 70 and 90 km. Within this narrow altitude-range of the ionosphere occur nearly all the effects that come under the heading of `sudden ionospheric disturbances' (S.I.D.).

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