Excitation of Atomic Ions of Astrophysical Interest by Electron Impact

Details Excitation of Atomic Ions of Astrophysical Interest by Electron Impact Excitation of Atomic Ions of Astrophysical Interest by Electron Impact

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.0303t&link_type=abstract

American Astronomical Society, AAS Meeting #212, #3.03; Bulletin of the American Astronomical Society, Vol. 40, p.184

Astronomy and Astrophysics

Astronomy

Scientific paper

Electron-ion collision processes play an important role in the understanding of energy balance in different types of astrophysical plasmas. Several line intensity ratios involving C II, O II, and Si II ions are density and/or temperature sensitive and can be used for diagnosing the physical conditions of planetary nebulae, seyfert galaxies, symbiotic stars, and solar transition region and corona. Electron collision excitation collision strengths for infrared, optical, and ultraviolet lines arising from transitions between the 42 levels of C II, 47 levels of O II, and 31-levels of Si II have been calculated using the B-spline Breit-Pauli R-matrix method. The relativistic effects have been incorporated in the Breit-Pauli Hamiltonian via the use of mass, Darwin, and spin-orbit operators. Flexible non-orthogonal orbitals in the multiconfiguration Hartree-Fock approach have been used to obtain accurate target description and to represent the scattering functions. Accurate scattering physical model includes a sophisticated target description and channel coupling between many channels to attain convergence. A B-spline basis is used for the description of continuum functions and no orthogonality constraint is imposed between the continuum functions and the valence spectroscopic and correlated atomic orbitals.
This research work is supported by NASA under grant NNG06GD39G from the Astronomy and Physics Research Analysis program.

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