Atomic data from the Iron Project. XXXVII. Electron impact excitation collision strengths and rate coefficients for Fe VI
Abstract
Collision strengths and Maxwellianaveraged rate coefficients have been calculated for 3 160 nonvanishing transitions among 80 fine structure levels, dominated by configurations 3d(3,) 3d(24) s, and 3d(24) p in Fe VI. Collision strengths are calculated using the Rmatrix method with a 34term closecoupling target expansion and for electron energies up to 10 Rydbergs. Detailed comparisons of rate coefficients are presented with the relativistic BreitPauli calculations using a 19level expansion corresponding to the first 8 LS terms dominated by the ground configuration 3d(3) . For the lowlying transitions of practical interest there is excellent agreement, better than 10%, among three sets of rate coefficients calculated using the 34term and 8term nonrelativistic calculations and the 19level BreitPauli calculation, indicating that (i) the relativistic effects are not too significant, and (ii) the numerical uncertainties associated with the resolution of the extensive resonances in the collision strengths are small. Rate coefficients are tabulated in a range of temperatures, 10(4)  10(6) K, where Fe VI is normally abundant in radiatively photoionized or collisionally ionized plasmas sources. A brief discussion of the calculations and sample results are given. The present rates for Fe VI are expected to find applications in UV spectral diagnostics of hot stellar sources and planetary nebulae. Table~4 for complete data for Fe~VI is only available in electronic form at the CDS via anonymous ftp to cdsarc.ustrasbg.fr (130.79.128.5) or via http://cdsweb.ustrasbg.fr/Abstract.html
 Publication:

Astronomy and Astrophysics Supplement Series
 Pub Date:
 April 1999
 DOI:
 10.1051/aas:1999464
 Bibcode:
 1999A&AS..136..395C
 Keywords:

 ATOMIC DATA;
 WHITE DWARFS;
 PLANETARY NEBULAE