J/MNRAS/414/713 Stark broadening of Sn III spectral lines (Alonso-Medina+, 2011)
Stark broadening of Sn III spectral lines of astrophysical interest:
predictions and regularities.
Alonso-Medina A., Colon C.
<Mon. Not. R. Astron. Soc., 414, 713-726 (2011)>
=2011MNRAS.414..713A 2011MNRAS.414..713A
ADC_Keywords: Atomic physics
Keywords: atomic data - atomic processes
Abstract:
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 SnIII 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
1023m-3 and temperatures T=11000-75000K. 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.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 57 238 *SnIII 4d105sns (n=6--9) results
table2.dat 57 280 *SnIII 4d105snp (n=5,6) and 4d105p2 results
table2b.dat 54 16 *SnIII 4d105snp (n=5,6) and 4d105p2 other
experimental values
table3.dat 57 504 *SnIII 4d105snd (n=5--7) results
table4.dat 57 176 *SnIII 4d105s4f and 4d105s5g results
table4b.dat 54 5 *SnIII 4d105s4f and 4d105s5g other
experimental values
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Note on table*.dat: for the Stark linewidth (FWHM) and line shift at an
electron density of 1017cm-3 (normalized to Ne=1023m-3).
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See also:
VI/82 : Stark broadening of H lines (Stehle 1995)
J/MNRAS/401/1080 : PbIV spectral lines Stark broadening (Alonso-Medina+, 2010)
Byte-by-byte Description of file: table1.dat table2.dat table3.dat table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq ? Line sequential number
4- 11 A8 --- Trans Transition array
13- 28 A16 --- Mult Multiplet
29- 35 F7.1 0.1nm lambda ? Wavelength (G1)
37- 40 F4.1 kK T [11.6,75] Temperature (G2)
42- 49 F8.3 pm omega Stark broadening linewidth ω at T
50- 57 F8.3 pm d Theoretical Stark line shift at T
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Byte-by-byte Description of file: table2b.dat table4b.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq ? Line sequential number
4- 11 A8 --- Trans Transition array
13- 27 A15 --- Mult Multiplet designation
29- 35 F7.1 0.1nm lambda ? Wavelength (G1)
37- 40 F4.1 kK T [11.6,75] Temperature (G2)
42- 46 F5.1 pm omega Stark broadening linewidth ω at T
48- 50 F3.1 pm d ? Theoretical Stark line shift at T
51- 52 I2 % e_omega ? Error on omega
54 A1 --- Ref Reference (2)
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Note (2): References as follows:
b = Kieft et al. (2004, Phys. Rev. E. 70, 066402)
c = Simic et al. (2008, Publ. Astron. Obs. Belgrade, 84, 487) -
the Sahal-Brechot approach
d = Simic et al. (2008, Publ. Astron. Obs. Belgrade, 84, 487) -
the Griem modified approach
e = Djenize (2007, Spectrochim. Acta B, 62, 403).
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Global notes:
Note (G1): from Moore, 1958, Atomic Energy Levels, NBS Circular 467,
Vol. III, Washington DC, p. 213
Note (G2): the grid of temperatures is made of the 8 values
(11.6, 17.5, 20, 25, 30, 35, 50, and 75)x103^K
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 19-Mar-2012