The Solar Spectrum: Wavelengths and Identifications from 60 TO 385 Angstroms

Abstract

The solar spectrum from 60 to 158 A and 163 to 385 - was photographed at a resolution of 004 A or better on glass plates The wavelengths of emission lines in these records were determined with a typical accuracy of 0.008 A above 100 A and 0.004 A below 100 A. The spectrograph employed a 3-meter radius, 1200 grooves gold grating at graxing incidence The design considerations and limitations of this instrument are presented along with a description of the Aerobee 130 flight mission on 1969 May t6. The wavelengths for the 370 observed lines are listed together with intensity estimates. Of these, the 180 identified lines are due to ions of lle, 0, Ne, Mg, Si, S, Ar, Ca, Fe, and Ni. These identified lines are also tabulated separately foi each isoelectronic sequence from Li I to K I. The solar lines are well enough resolved that wavelength determinations to t 0.004 A can be made whenever better laboratory wavelengths become available. The reliability of the solar line "Mentifications" could then be much improved.