Interstellar gas studies in the balloon ultraviolet

Details Interstellar gas studies in the balloon ultraviolet Interstellar gas studies in the balloon ultraviolet

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975rspta.279..303b&link_type=abstract

(Royal Society, Discussion on Astronomy in the Ultraviolet, London, England, Apr. 9, 10, 1974.) Royal Society (London), Philosop

Astronomy and Astrophysics

Astronomy

11

Balloon-Borne Instruments, Interstellar Gas, Line Spectra, Stellar Spectra, Ultraviolet Spectroscopy, Abundance, Electron Density (Concentration), Magnesium, Photoionization, Stabilized Platforms, Tables (Data)

Scientific paper

Spectral observations at a resolution of 0.1 A covering the region from 2870 to 2740 A have been made of several stars with an objective grating spectrograph mounted on a balloon-borne star-stabilized platform. Measurements are reported of the interstellar lines of Mg II at 2795.53 A and 2802.70 A and Mg I at 2852.13 A. It is noted that in the general (H I) interstellar medium, Mg is predominantly in the Mg(+) state, so its interstellar abundance can be determined directly from the Mg II lines if the position on the curve of growth is known, and that observation of both Mg(+) and neutral Mg gives information on the ionization balance and leads to a value for the interstellar electron density. Values for the interstellar Mg abundance and electron density are derived for the gas in the directions of the stars observed. The results indicate that the predominant ionizing mechanism in cool clouds is photoionization by starlight.

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