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J/A+A/606/A11       Inelastic e+Mg collision data            (Barklem+, 2017)

Inelastic e+Mg collision data and its impact on modelling stellar and supernova spectra. Barklem P.S., Osorio Y., Fursa D.V., Bray I., Zatsarinny O., Bartschat K., Jerkstrand A. <Astron. Astrophys. 606, A11 (2017)> =2017A&A...606A..11B (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics Keywords: atomic data - atomic processes Abstract: Results of calculations for inelastic e+Mg effective collision strengths for the lowest 25 physical states of MgI (up to 3s6p1P), and thus 300 transitions, from the convergent close-coupling (CCC) and the B-spline R-matrix (BSR) methods are presented. At temperatures of interest, ∼5000K, the results of the two calculations differ on average by only 4%, with a scatter of 27%. As the methods are independent, this suggests that the calculations provide datasets for e+Mg collisions accurate to this level. Comparison with the commonly used dataset compiled by Mauas et al. (1988ApJ...330.1008M), covering 25 transitions among 12 states, suggests the Mauas et al. data are on average ∼57% too low, and with a very large scatter of a factor of ∼6.5. In particular the collision strength for the transition corresponding to the MgI intercombination line at 457nm is significantly underestimated by Mauas et al., which has consequences for models that employ this dataset. In giant stars the new data leads to a stronger line compared to previous non-LTE calculations, and thus a reduction in the non-LTE abundance correction by ∼0.1dex (∼25%). A non-LTE calculation in a supernova ejecta model shows this line becomes significantly stronger, by a factor of around two, alleviating the discrepancy where the 457nm line in typical models with Mg/O ratios close to solar tended to be too weak compared to observations. Description: The file states.dat lists the considered states. The remaining files then provide the effective collision strength matrices for various temperatures from the convergent close coupling (CCC) and B-spline R-matrix (BSR) calculations. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file states.dat 25 25 States and their energies 500k_b.dat 250 25 BSR data for 500 K 1000k_b.dat 250 25 BSR data for 1000 K 2000k_b.dat 250 25 BSR data for 2000 K 3000k_b.dat 250 25 BSR data for 3000 K 4000k_b.dat 250 25 BSR data for 4000 K 5000k_b.dat 250 25 BSR data for 5000 K 6000k_b.dat 250 25 BSR data for 6000 K 7000k_b.dat 250 25 BSR data for 7000 K 8000k_b.dat 250 25 BSR data for 8000 K 9000k_b.dat 250 25 BSR data for 9000 K 10000k_b.dat 250 25 BSR data for 10000 K 15000k_b.dat 250 25 BSR data for 15000 K 20000k_b.dat 250 25 BSR data for 20000 K 500k_c.dat 250 25 CCC data for 500 K 1000k_c.dat 250 25 CCC data for 1000 K 2000k_c.dat 250 25 CCC data for 2000 K 3000k_c.dat 250 25 CCC data for 3000 K 4000k_c.dat 250 25 CCC data for 4000 K 5000k_c.dat 250 25 CCC data for 5000 K 6000k_c.dat 250 25 CCC data for 6000 K 7000k_c.dat 250 25 CCC data for 7000 K 8000k_c.dat 250 25 CCC data for 8000 K 9000k_c.dat 250 25 CCC data for 9000 K 10000k_c.dat 250 25 CCC data for 10000 K 15000k_c.dat 250 25 CCC data for 15000 K 20000k_c.dat 250 25 CCC data for 20000 K
See also: J/A+A/572/A103 : Inelastic silicon-hydrogen collision data (Belyaev+, 2014) J/A+A/587/A114 : Inelastic calcium-hydrogen collision data (Bellyaev+, 2016) J/A+A/593/A27 : Inelastic beryllium-hydrogen collision data (Yakovleva+, 2016) Byte-by-byte Description of file: states.dat
Bytes Format Units Label Explanations
2- 3 I2 --- Index [1/25] Index 8- 14 A7 --- Label Term label 17- 18 I2 --- g Statistical weight 21- 25 F5.3 eV E Term energy in eV
Byte-by-byte Description of file: *_b.dat *_c.dat
Bytes Format Units Label Explanations
3- 10 E8.2 --- Upsilon1 Effective collision strengths matrix (1) 13- 20 E8.2 --- Upsilon2 Effective collision strengths matrix (1) 23- 30 E8.2 --- Upsilon3 Effective collision strengths matrix (1) 33- 40 E8.2 --- Upsilon4 Effective collision strengths matrix (1) 43- 50 E8.2 --- Upsilon5 Effective collision strengths matrix (1) 53- 60 E8.2 --- Upsilon6 Effective collision strengths matrix (1) 63- 70 E8.2 --- Upsilon7 Effective collision strengths matrix (1) 73- 80 E8.2 --- Upsilon8 Effective collision strengths matrix (1) 83- 90 E8.2 --- Upsilon9 Effective collision strengths matrix (1) 93-100 E8.2 --- Upsilon10 Effective collision strengths matrix (1) 103-110 E8.2 --- Upsilon11 Effective collision strengths matrix (1) 113-120 E8.2 --- Upsilon12 Effective collision strengths matrix (1) 123-130 E8.2 --- Upsilon13 Effective collision strengths matrix (1) 133-140 E8.2 --- Upsilon14 Effective collision strengths matrix (1) 143-150 E8.2 --- Upsilon15 Effective collision strengths matrix (1) 153-160 E8.2 --- Upsilon16 Effective collision strengths matrix (1) 163-170 E8.2 --- Upsilon17 Effective collision strengths matrix (1) 173-180 E8.2 --- Upsilon18 Effective collision strengths matrix (1) 183-190 E8.2 --- Upsilon19 Effective collision strengths matrix (1) 193-200 E8.2 --- Upsilon20 Effective collision strengths matrix (1) 203-210 E8.2 --- Upsilon21 Effective collision strengths matrix (1) 213-220 E8.2 --- Upsilon22 Effective collision strengths matrix (1) 223-230 E8.2 --- Upsilon23 Effective collision strengths matrix (1) 233-240 E8.2 --- Upsilon24 Effective collision strengths matrix (1) 243-250 E8.2 --- Upsilon25 Effective collision strengths matrix (1)
Note (1): The matrices follow the ordering of indexes in states.data; i.e. the transition 1-2 corresponds to element (1,2), noting the matrix is symmetric.
Acknowledgements: Paul Barklem, paul.barklem(at)physics.uu.se
(End) Paul Barklem [Uppsala Univ., Sweden], Patricia Vannier [CDS] 19-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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