Abstract
Using Griem’s semi-empirical approach, we have calculated the Stark broadening parameters (line widths and shifts) of 35 UV–Blue spectral lines of neutral vanadium (V I). These lines have been detected in the Sun, the metal-poor star HD 84937, and Arcturus, among others. In addition, these parameters are also relevant in industrial and laboratory plasma. The matrix elements required were obtained using the relativistic Hartree–Fock (HFR) method implemented in Cowan’s code.
Highlights
Chemical elements belonging to the iron group, from Scandium to Zirconium (Z = 21–30), are critical for an understanding of nucleosynthesis in different super-nova types
Vanadium is produced by explosive silicon burning and oxygen burning in the core-collapse supernova (SN) phase [1]
Among all the effects that have an impact on atomic spectral lines, the knowledge of the broadening and shift produced by charged particles is essential
Summary
Vanadium (together with Scandium and Titanium) is produced by explosive silicon burning and oxygen burning in the core-collapse supernova (SN) phase [1]. In recent works, this element has been analyzed in detail, especially in metal-poor stars [2]. Accurate measurements of Stark broadening and shift parameters are required to properly analyze astrophysical data. In the case of Vanadium, Manrique et al [4] have provided experimental information related to the Stark broadening and shift parameters of the spectral lines of ionized Vanadium (V II)
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