The atomic model of the Sn plasmas for the EUV source

Sasaki, Akira; Sunahara, A.; Nishihara, Katsunobu; Nishikawa, Takeshi; Koike, Fumihiro; Tanuma, H.

doi:10.1088/1742-6596/163/1/012107

Cited by 5 publications

(5 citation statements)

References 6 publications

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“…In all ion stages these transitions give rise to the strongest peak, with the ∆n > 0 transitions not influencing the peak emission greatly. Previous studies on Sn and Xe reported that the resonant transition contribution to emission is greatly enhanced by the presence of satellite lines 8,19,20 . The inclusion of doubly excited states in Gd and Tb will be considered in a future work.…”

Section: B Distribution Of Line Strengthsmentioning

confidence: 95%

Extreme ultraviolet emission spectra of Gd and Tb ions

Kilbane

O'Sullivan

2010

Journal of Applied Physics

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Theoretical EUV emission spectra of gadolinium and terbium ions calculated with the Cowan suite of codes and the FAC relativistic code are presented. 4d−4f and 4p−4d transitions give rise to unresolved transition arrays in a range of ions. The effects of configuration interaction are investigated for transitions between singly excited configurations. Optimization of emission at 6.775 nm and 6.515 nm is achieved for Gd and Tb ions respectively by consideration of plasma effects. The resulting synthetic spectra are compared with experimental spectra recorded using the laser produced plasma technique.

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Section: B Distribution Of Line Strengthsmentioning

confidence: 95%

Extreme ultraviolet emission spectra of Gd and Tb ions

Kilbane

O'Sullivan

2010

Journal of Applied Physics

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“…Simić et al (2008) and Simi (2009) investigated theoretically the influence of collisions with charged particles on heavy metal spectral‐line profiles for Sn iii in the spectra of A stars and white dwarfs. Also, Sn plasmas are being intensively studied as a candidate for the extreme ultraviolet light source for next‐generation microlithography (Harilal, O'Shay & Tillack 2005; Sasaki et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Stark broadening of Sn iii spectral lines of astrophysical interest: predictions and regularities

Alonso‐Medina

Colón

2011

Monthly Notices of the Royal Astronomical Society

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The determination of the Stark broadening parameters of Sn ions is useful for astrophysicists interested in the determination of the density of electrons in stellar atmospheres. In this paper, we report on the calculated values of the Stark broadening parameters for 171 lines of Sn iii arising from 4d105sns (n= 6–9), 4d105snp (n= 5, 6), 4d105p2, 4d105snd (n= 5–7), 4d105s4f and 4d105s5g. Stark linewidths and line shifts are presented for an electron density of 1023 m−3 and temperatures T= 11 000–75 000 K. These have been calculated using a semi‐empirical approach, with a set of wavefunctions obtained from Hartree–Fock relativistic calculations, including core polarization effects. The results obtained have been compared with available experimental data. These can be used to consider the influence of Stark broadening effects in A‐type stellar atmospheres.

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“…Recently the needs for experimental databases of extreme ultraviolet (EUV) radiation from highly charged tin (Sn) ions have been increasing. Sn plasmas are being intensively studied [1][2][3] as a candidate of extreme ultra-violet (EUV) light source for the next generation microlithography [4,5]. In astrophysical applications, information about the transition probabilities and lifetimes can be used to determine elemental abundances from absorption spectra.…”

Section: Introductionmentioning

confidence: 99%

Calculation of oscillator strengths, transition probabilities and radiative lifetimes of levels in Sn III

Colón¹,

Alonso‐Medina²

2010

J. Phys. B: At. Mol. Opt. Phys.

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Abstract. This paper contains the results of theoretical calculations of oscillator strengths and transition probabilities of 171 spectral lines arising from 4d 10 5sns (n=6-9), 4d 10 5snp (n=5,6), 4d 10 5p 2 , 4d 10 5snd(n=5-7), 4d 10 5s4f and 4d 10 5s5g configurations and 36 level radiative lifetimes of Sn III has been calculated. These values were obtained in intermediate coupling (IC) and using relativistic Hartree-Fock calculations including core-polarization effects in the potential and the corresponding corrections in the matrix elements. We use for the IC calculations the standard method of least square fitting from experimental energy levels by means of Cowan computer code. The inclusion in these calculations of the 4d 9 5s 2 5p has facilitated us a new assignment of the levels of energy in the Sn III. Transition probabilities, oscillator strengths and radiative lifetimes obtained are in good agreement with the experimental data.

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The atomic model of the Sn plasmas for the EUV source

Cited by 5 publications

References 6 publications

Extreme ultraviolet emission spectra of Gd and Tb ions

Extreme ultraviolet emission spectra of Gd and Tb ions

Stark broadening of Sn iii spectral lines of astrophysical interest: predictions and regularities

Calculation of oscillator strengths, transition probabilities and radiative lifetimes of levels in Sn III

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