Abstract
The shapes of the astrophysically interesting neutral manganese (Mn I) resonance spectral lines (403.075, 403.306, 403.448, 279.481, 279.826 and 280.108 nm) have been observed together with six other prominent Mn I lines in the laboratory helium plasma at a 47 000 K electron temperature and 6.6 × 10 22 m - 3 electron density. With these plasma parameters the Stark broadening has been found to be an important mechanism in the Mn I line shape formation. Our measured Mn I Stark widths ( W ) are the first data in the literature. Stark widths are compared with line hyperfine structure splittings ( Δ hfs ). At above mentioned helium plasma conditions the line broadening due to hyperfine structure splitting of the lines is less than that of the Stark and Doppler broadening for the case of the Mn I lines under investigation. We estimate that at electron densities below 10 20 m - 3 and electron temperatures below 4000 K the components in the hyperfine structure play an important role in the mentioned Mn I line shape formation.
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