Free Access
Issue
Astron. Astrophys. Suppl. Ser.
Volume 136, Number 2, April II 1999
Page(s) 395 - 403
DOI https://doi.org/10.1051/aas:1999464
Published online 15 April 1999
DOI: 10.1051/aas:1999464

Astron. Astrophys. Suppl. Ser. 136, 395-403

Atomic data from the Iron Project

XXXVII. Electron impact excitation collision strengths and rate coefficients for Fe VI[*]

G.X. Chen and A.K. Pradhan

Send offprint request: G.-X. Chen

Department of Astronomy, The Ohio State University, Columbus, OH 43210, U.S.A. Internet: chen@astronomy.ohio-state.edu

Received November 20; accepted January 14, 1999

Abstract:

Collision strengths and Maxwellian-averaged rate coefficients have been calculated for 3 160 non-vanishing transitions among 80 fine structure levels, dominated by configurations $3{\rm d}^3, 3{\rm d}^24{\rm s}$, and $3{\rm d}^24$p in Fe VI. Collision strengths are calculated using the R-matrix method with a 34-term close-coupling target expansion and for electron energies up to 10 Rydbergs. Detailed comparisons of rate coefficients are presented with the relativistic Breit-Pauli calculations using a 19-level expansion corresponding to the first 8 LS terms dominated by the ground configuration $3{\rm d}^3$. For the low-lying transitions of practical interest there is excellent agreement, better than 10%, among three sets of rate coefficients calculated using the 34-term and 8-term non-relativistic calculations and the 19-level Breit-Pauli 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, 104 - 106 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.

Key words: atomic data -- white dwarfs -- planetary nebulae


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