Physical conditions in the cool parts of prominences

Details Physical conditions in the cool parts of prominences Physical conditions in the cool parts of prominences

Jul 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...270..265l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 270, July 1, 1983, p. 265-269.

Astronomy and Astrophysics

Astrophysics

16

Solar Prominences, Solar Spectra, Balmer Series, Hydrogen Ions, Resonance Lines, Sodium, Strontium

Scientific paper

A spectral analysis of the cool parts of seven prominences reported by Shin-Huei (1961) and Yakovkin and Zel'dina (1964) is presented. The analysis requires only measurements of the Na and Sr(+) resonance lines and the middle H Balmer lines, all of which are optically thin, and uses the Na and Sr(+) statistical equilibrium solutions of Landman (1983). It is shown that the Na/H integrated intensity ratios alone are sufficient to determine the degree of H ionization. The major result of this investigation is that the degree of H ionization in the cool prominence parts is very low and the total gas pressure very high.

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