Emission lines in the spectrum of Io

Details Emission lines in the spectrum of Io Emission lines in the spectrum of Io

Jul 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978avest..12...27a&link_type=abstract

(Astronomicheskii Vestnik, vol. 12, Jan.-Mar. 1978, p. 27-33.) Solar System Research, vol. 12, no. 1, July 1978, p. 21-26. Tran

Astronomy and Astrophysics

Astrophysics

Astronomical Spectroscopy, Atmospheric Composition, D Lines, Emission Spectra, Io, Jupiter Atmosphere, Calcium, Graphs (Charts), Iron, Magnesium, Potassium, Sodium, Spectrograms

Scientific paper

Spectrograms of Io obtained with the 2-m reflector at the Shemakha Astrophysical Observatory, at dispersions of 12 and 15 A/mm have been used to study profiles of Na I, Fe I, Mg I, and Ca I emission lines. The line profiles were found to be asymmetric. It is shown that variations of the intensity ratio D2/D1 in the spectrum of Io do in fact occur, varying within the limits 1.6 plus or minus 0.3. The intensity of the sodium D-line at Phi = 90 deg is about 40% higher than at Phi = 270 deg. The number of radiating neutral sodium atoms and the lower limit of the number of radiating iron, magnesium, and potassium atoms along the line of sight are calculated.

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