Abstract
ABSTRACT We have measured the Stark widths and shifts of V II spectral lines in the wavelength range 2000–4200 Å belonging to 75 multiplets. The spectra are emitted by laser-induced plasmas generated from fused glass discs prepared by borate fusion. The electron density and temperature are in the ranges (0.72–6.5) × 1017 cm−3 and (11 000–14 900) K, respectively. To avoid self-absorption, we have used seven samples with vanadium concentrations selected by the CSigma graph methodology. This has allowed to include strong and weak lines in the study, including resonance and forbidden lines. The experimental widths and shifts are compared with theoretical values available in the literature.
Highlights
The knowledge of the broadening and shift produced by charged particles on the spectral lines is essential for spectroscopic diagnostic and atomic structure calculations
An additional spectrum with 7 μs delay is used as a reference to obtain the Stark shifts, as the electron density has decreased to a negligible value at this late time of the plasma evolution
Matrix effects could lead to a non-negligible variation of the electron density among the plasmas generated with the different samples
Summary
The knowledge of the broadening and shift produced by charged particles on the spectral lines is essential for spectroscopic diagnostic and atomic structure calculations. Accurate measurements of Stark broadening and shift parameters are required in laboratory plasma research, atomic structure calculations, and to analyse astrophysical data. A large number of ionized vanadium spectral lines has been observed in stellar objects and solar plasma, being overabundant in some A-type stars (van’t Veer-Mennert et al 1985; Sadakane & Ueta 1989), where the Stark broadening is the main pressure broadening mechanism. Despite the interest of these applications, there are no accurate V II Stark width and shifts measurements and very few theoretical calculations. Wood et al (2014) have reported new experimental transition probability values for V II transitions, highlighting the need to measure simultaneously strong and very week lines in laboratory to explain unexpected trends in stellar abundance determinations
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