Electron Collision and Photoionization Cross Sections for Ions of Astrophysical Interest

Details Electron Collision and Photoionization Cross Sections for Ions of Astrophysical Interest Electron Collision and Photoionization Cross Sections for Ions of Astrophysical Interest

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.1902t&link_type=abstract

American Astronomical Society Meeting 208, #19.02; Bulletin of the American Astronomical Society, Vol. 38, p.100

Astronomy and Astrophysics

Astrophysics

Scientific paper

Electron collision excitation rates, oscillator strengths, and photoionization cross sections of ions of astrophysical interest are needed to model a wide range of astrophysical objects such as planetary nebulae, H II regions, active galactic nuclei, novae, and supernovae. Oscillator strengths for the UV and FUV lines are needed to study absorption by gases in the interstellar and intergalactic mediums. Accurate representation of target wave functions that properly account for the important correlation and relaxation effects and inclusion of coupling effects are essential components of a reliable collision calculation. The effect of coupling to the continuum is included through the use of pseudo-states that are chosen to account for most of the dipole polarizabilities of target states. Non-orthogonal orbitals technique in multiconfiguration Hartree-Fock approach is used to calculate oscillator strengths and transition probabilities. Comparison of the computed excitation energies and oscillator strengths with experiment can provide a check on the accuracy of target wave functions. The B-spline basis is used in the R-matrix approach to calculate electron excitation collision strengths and photoionization cross sections. Recent results for oscillator strengths, electron excitation collision strengths, and photoionization for transitions in N I, O II, O IV, S II, and Fe XIV will be presented.This research work is supported by NASA Grant Number NNG06GD39G.

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