The effect of hyperfine splitting on Stark broadening for three blue-green Cu i lines in laser-induced plasma

Abstract

Stark effect is observed in many natural and artificial plasmas and is of great importance for diagnostic purposes. Since this effect alters profiles of spectral lines, it should be taken into account when assessing chemical composition of radiation sources, including stars. Copper is one of the elements which studies of stellar atmospheres deal with. To this end, UV and visible Cu lines are used. However, there is a lack of agreement between existing data on their Stark parameters. It is therefore of interest to obtain new experimental data on these lines and to compare them to previous results. In this work, we have estimated Stark widths and shifts for three blue-green lines at 5105.54, 5153.24, and 5218.20 Å (corresponding transitions are [3d 10 4p] 2 P° → [3d 9 4s 2 ] 2 D and [3d 10 4d] 2 D → [3d 10 4p] 2 P°) observed in a "long-spark" laser-induced plasma. For the first time, we have accurately estimated an impact of hyperfine splitting on the profile shapes of the studied lines taking also into account the isotope shifts. We have shown that both effects considerably influence shift and width of Cu I line at 5105.54 Å, and shifts of Cu I lines at 5153.24 and 5218.20 Å.

Feasibility of Using Boltzmann Plots to Evaluate the Stark Broadening Parameters of Cu(I) Lines

“…1,5,6,8,10 Several authors calculated the Stark broadening parameters of several transition lines for the copper and some other elements using different techniques. 7,[26][27][28][29][30][31] In this paper, we shall confirm the feasibility of using the Boltzmann plot to estimate the missing values of Stark broadening parameters of the three Cu(I) lines at wavelength transitions of 330.79, 359.91, and 360.2 nm.…”

Controlling the plasma electron number density of copper metal using NIR picosecond laser-induced plasma spectroscopy

“…Assuming LTE conditions, as well be verified later, the electron density is considered by adopting Boltzmann distribution of the electron density as follows [19,20]: (1) where N e is the electron density (in cm -3 ), Δλ FWHM is the fundamental line width at half maximum and W e is the electron impact parameter (Stark broadening value). The average value of the W e for Cu I 521.8 nm is 0.180 nm, as given by previous work POPOV et al [21]. The Stark line width Δλ FWHM can be corrected by subtracting the instrumental (Δλ instrument ) from the observed line width (Δλ observed ) as follows [22]:…”

Forty Years of the Applications of Stark Broadening Data Determined with the Modified Semiempirical Method

“…Of particular interest were data on Stark broadening of Cu II lines [87]. They were used in articles considering dependence of laser fluence on dynamics of emission of copper plasma induced by ultrafast laser [109], the effect of uniform magnetic field on it and the particles deposited on the surface of target [110], studies of time-integrated optical emission for Cu plasma in air at atmospheric pressure with magnetic field [112], radiation decay constant dependence on focal position for copper plasma [116], the effect of hyperfine structure on Stark broadening in the case of three blue-green Cu spectral lines in plasma induced by laser [118], enhancement of signal intensity using cavity confinement of plasma produced by a laser [114], the study of temporal evolution of plasma induced by CO 2 pulsed laser on targets made of titanium oxides [99], the mechanism of effect of distance between a lens and a sample on plasma induced by laser [100], and the effect of ambient pressure on titanium plasma induced by a femtosecond laser [101].…”