Spectral line ratios

The analysis of line intensity ratios is an important tool to obtain information about laboratory and space plasmas. In emission spectroscopy, the intensity of spectral lines can provide various information about the plasma (or gas) condition. It might be used to determine the temperature or density of the plasma. Since the measurement of an absolute intensity in an experiment can be challenging, the ratio of different spectral line intensities can be used to achieve information about the plasma, as well.

Theory

The emission intensity density of an atomic transition from the upper state to the lower state is:^[1]

$P_{u\rightarrow l}=N_{u}\ \hbar \omega _{u\rightarrow l}\ A_{u\rightarrow l}$

where:

$N_{u}$ is the density of ions in the upper state,
$\hbar \omega _{u\rightarrow l}$ is the energy of the emitted photon, which is the product of the Planck constant and the transition frequency,
$A_{u\rightarrow l}$ is the Einstein coefficient for the specific transition.

The population of atomic states N is generally dependent on plasma temperature and density. Generally, the more hot and dense the plasma, the more the higher atomic states are populated. The observance or not-observance of spectral lines from certain ion species can, therefore, help to give a rough estimation of the plasma parameters.

More accurate results can be obtained by comparing line intensities:

${\frac {P_{u_{1}\rightarrow l_{1}}}{P_{u_{2}\rightarrow l_{2}}}}={\frac {N_{u_{1}}\omega _{u_{1}\rightarrow l_{1}}A_{u_{1}\rightarrow l_{1}}}{N_{u_{2}}\omega _{u_{2}\rightarrow l_{2}}A_{u_{2}\rightarrow l_{2}}}}$

The transition frequencies and the Einstein coefficients of transitions are well known and listed in various tables as in NIST Atomic Spectra Database. It is often that atomic modeling^[2] is required for determination of the population densities $N_{u_{1}}$ and $N_{u_{2}}$ as a function of density and temperature. While for the temperature determination of plasma in thermal equilibrium Saha's equation and Boltzmann's formula might be used, the density dependence usually requires atomic modeling.

External links

NIST Atomic Spectra Database

References

^ Salzmann, D. (1998). Atomic Physics in Hot Plasmas. Oxford University Press. p. 149. ISBN 978-0-19-510930-6.
^ Ralchenko, Yu. V.; Maron, Y. (2001). "Accelerated recombination due to resonant deexcitation of metastable states". J. Quant. Spectr. Rad. Transfer. 71 (2–6): 609–621. arXiv:physics/0105092. Bibcode:2001JQSRT..71..609R. CiteSeerX 10.1.1.74.3071. doi:10.1016/S0022-4073(01)00102-9. S2CID 17090954.

Latimer, I; Mills, JI; Day, RA (1970), "Refinements in the helium line ratio technique for electron temperature measurement and its application to the precursor", Journal of Quantitative Spectroscopy and Radiative Transfer, 10 (6), Elsevier: 629–635, Bibcode:1970JQSRT..10..629L, doi:10.1016/0022-4073(70)90079-8
Muñoz Burgos, JM; Barbui, T; Schmitz, O; Stutman, D; Tritz, K (2016), "Time-dependent analysis of visible helium line-ratios for electron temperature and density diagnostic using synthetic simulations on NSTX-U", Review of Scientific Instruments, 87 (11), AIP: 11E502, doi:10.1063/1.4955286, OSTI 1259296

[1] Salzmann, D. (1998). Atomic Physics in Hot Plasmas. Oxford University Press. p. 149. ISBN 978-0-19-510930-6.

[2] Ralchenko, Yu. V.; Maron, Y. (2001). "Accelerated recombination due to resonant deexcitation of metastable states". J. Quant. Spectr. Rad. Transfer. 71 (2–6): 609–621. arXiv:physics/0105092. Bibcode:2001JQSRT..71..609R. CiteSeerX 10.1.1.74.3071. doi:10.1016/S0022-4073(01)00102-9. S2CID 17090954.

[1]

[2]

Theory

See also

External links

References