Effect of modulated high-pressure mercury discharges on the shape of self-reversed lines

Abstract

The variation of the principal characteristics of the mercury visible triplet self-reversed lines is studied as a function of radial and temporal profiles of the temperature and of the species densities in high pressure mercury discharges (∼2 and ∼3 atm) operating on 50 Hz ac. An investigation is made into the effect of different theoretical and experimental parameters on the shape of calculated self-reversed lines. By comparison between experimental and theoretical results an estimation is made of the broadening constants and of the transition probabilities of the lines.

Determination of the radial temperature profile in a high-pressure mercury discharge using the electrical conductivity

“…The radiance of optically thin mercury lines (577/579 nm) is used to determine the radial temperature profile around the discharge axis [1,2].…”

“…In our case the lines HgI (λ (1) = 576.96 nm; 6 3 D 2 -6 1 P 1 ) and HgI (λ (2) = 579.07 nm; 6 1 D 2 , 6 3 D 1 -6 1 P 1 ) are used, and they are optically thin (cf also [5,6]). Because these two lines are superimposed, the resulting spectral emission coefficient is 1) g (1) m A (1) mn exp…”

“…The advantage of this standard is its intensive radiation in the examined spectral region. The received The spectral radiance density distribution of the mercury discharge with the wavelengths λ (1) and λ (2) in the discharge axis.…”

Application of the hook method and emission spectroscopy for the determination of radial density and temperature profiles in high-pressure mercury discharges

“…The radiance of optically thin mercury lines (577.0/579.1 nm) is used to determine the radial temperature profile in the discharge axis [5,10]. The spectral emission coefficient ε ki of a line is given by [11]…”

“…Special attention is paid to the radial behaviour and to absolute quantities of the mercury triplet states 6 3 P 0 , 6 3 P 1 and 6 3 P 2 and the ground state 6 1 S 0 . The used absorption lines at 404.7, 435.8, 546.1 and 253.7 nm are optically thick [5,6].…”