EUV Beam-Foil Spectra of Scandium, Vanadium, Chromium, Manganese, Cobalt, and Zinc

Abstract

Beam-foil extreme-ultraviolet spectra of Sc, V, Cr, Mn, Co and Zn are presented that provide survey data of a single element exclusively. Various details are discussed in the context of line intensity ratios, yrast transitions, delayed spectra and peculiar properties of the beam-foil light source.

EUV Beam-Foil Spectra of Titanium, Iron, Nickel, and Copper

“…The beam-foil measurement technique has been recalled in various reviews (see [61,62] and references therein) and in two recent companion papers [30,31]. The spectra shown in this study have been obtained at the Bochum Dynamitron tandem accelerator laboratory (DTL), where a 4 MV tandem accelerator equipped with a sputter ion source [63,64] provided ion beams of more than 40 elements, with an energy from a few MeV up to about 30 MeV, and with beam currents (particle current) in the range from 0.1 µA to several µA of most iron group elements.…”

“…Besides Fe (Z = 26), the other even-numbered elements of the iron group (Ti (Z = 22), Cr (Z = 24), and Ni (Z = 28)) have been studied mostly in terrestrial spectra, although their abundance allows for expecting some prominence also in astrophysical spectra. Of these, Cr has been covered in a recent companion paper [31]. On the other hand, the odd-numbered element Cu (Z = 29) is not very abundant in space and thus not prominent in astrophysical spectra.…”

“…Figure 16 shows samples of prompt and delayed spectra of foil-excited Fe ion beams. In Reference [31], it has been discussed how the isotope-pure beam-foil light source suffers from a scarcity of wavelength reference lines in many spectra, especially in delayed ones. In prompt spectra (with reference lines), the signal of the decays of long-lived levels is too weak to be seen against the competition by short-lived level decays.…”

“…However, the latter technique provides isotopically pure spectra and thus can contribute to the analysis of coronal EUV spectra even if the spectral resolution is typically poorer than that of the spacecraft spectrographs. This contribution of data are one of the goals of the present study and its companions (on K and C [30], and on Sc, V, Cr, Mn, Co, Zn [31]) which together span the range of elements from Z = 19 to 30.…”