Detection Method of H 21 CM and Other Lines in the Radio Spectrum of the Sun.
Final scientific rept. 1 Jan 67-30 Jun 69,
OSSERVATORIO ASTROFISICO DI ARCETRI FLORENCE (ITALY)
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The work essentially investigates the intensity of the hydrogen 3 cm. and 21 cm. lines in the solar spectrum. A form of the transfer equation suitable for the high precision required, is found together with a technique for avoiding, in its integration, the singularity at the turning point. The method followed to calculate the populations is described and the transition rate coefficients are discussed. A model of the atmosphere is presented and the populations of the levels n 1, 2P12, 2S12, 2P32, n 3, n 4 of the hydrogen atom are found, as functions of the height above the photosphere. The population equilibrium of the most important states in the chromosphere, in the transition region and in the corona is discussed, and, finally, the intensity of the 3 cm line is calculated it turns out to be too small to be detected. An analogous procedure, relative to the 21 cm line, is followed for a cold quiet prominence. Author