Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...418..363t&link_type=abstract
Astronomy and Astrophysics, v.418, p.363-369 (2004)
Astronomy and Astrophysics
Astrophysics
3
Atomic Data, Atomic Processes, Line: Formation
Scientific paper
The B-spline basis has been used in the R-matrix approach to calculate electron impact excitation collision strengths for transitions between the 3s23p4 3P0,1,2, 1D2 and 1S0 levels and from these levels to the fine-structure levels of the excited 3s3p5, 3s23p34s, 3s23p33d, 3s23p34p and 3s23p34d configurations of Cl II. We considered 23 LS states 3s23p4 3P, 1D, 1S, 3s3p5 3P°, 3s23p3(4S°)4s 5,3S°, 3s23p3(4S°)3d 5,3D°, 3s23p3(2D°)3d 1P°, 1S°, 3F°, 3D°, 3P°, 3s23p3(2D°)4s 3,1D°, 3s23p3(2P°)4s 3,1P°, 3s23p3(4S°)4p 5,3P, 3s23p3(2P°)3d 3,1P°, 3D° and 3s23p3(2D°)4d 3P° in the close-coupling expansion that give rise to 51 fine-structure levels. The non-orthogonal orbitals are used for an accurate representation of both the target wavefunctions and the R-matrix basis functions. The collision strengths for transitions between fine-structure levels are calculated by transforming the LS-coupled K-matrices to K-matrices in an intermediate coupling scheme. The Rydberg series of resonances converging to excited state thresholds make substantial contributions to collision strengths. The thermally averaged collision strengths have been obtained by integrating collision strengths over a Maxwellian distribution of electron energies and these are listed in Table 2 for log T from 3.3 to 5.6 K.
Table 2 is only available in electronic form at CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/418/363
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