Excitation Potential in Solar Phenomena

Abstract

view Abstract Citations References Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Excitation Potential in Solar Phenomena St. John, C. E. Abstract i. Excitalion potential fixes the relative heights of the effective absorbing layers above the photosphere. High values of excitation potential require the stronger fields of excitation obtaining near the photosphere in order to excite the needed number of atoms to the energy-levels of absorption (Table I). 2. Low heights above the photosphere of absorbing layers for multiplets with high excitation potential are shown by correlating excitation potential with outflow from spots, heights from flash spectra, red displacement, and line intensity, in graphs i, 2, 3 of Figure i. ~. The absorbing layers for intersystem lines of a given excitation potential are nearer the photosphere than those for normal lines of the same excitation potential (Table V). The low transition probability for intersystem lines requires the greater abundance of atoms obtaining at the higher pressure near the photosphere. 4. Excitation potential determines (i) the possibility and relative probabifity of the occurrence of a line in the sun's spectrum; (2) the relative heights of absorbing layers above the photosphere; (~) in connection with transition probability, the maximum line intensity in a multiplet; and (~) the temperature classification (Table VI). ~. Small changes in the energy-level of the higher term are associated with profotmd changes in the character of the lines and furnish the basis for a fundamental classifica- tion (Table VII) Publication: The Astrophysical Journal Pub Date: December 1929 DOI: 10.1086/143228 Bibcode: 1929ApJ....70..319S full text sources ADS | Related Materials (1) Reprint: 1929CMWCI.390....1S