EXCITATION WITHIN THE GROUND CONFIGURATION OF O-LIKE IONS INDUCED BY PROTON IMPACT

S.L. Campbell and R.H.G. Reid

Department of Applied Mathematics and Theoretical Physics, Queen's University Belfast

The main interest is in the fine-structure transitions 2s22p4 3PJ →2s22p4 3PJ' . A symmetrized close-coupled semi-classical method is used, with the proton following hyperbolic trajectories, as described by Alder and Winther [1] and Ryans et al [2].
Several approximations for the radial factor of the interaction matrix elements are tested. The scaled-hydrogenic approximation [2], has the virtue of giving analytic expressions. More accurate HF radial orbitals were also considered. The changes to the cross sections are slight.
The effect of allowing, via a polarization potential, for dipole-coupling between the ground 2s22p4 configuration and the 2s2p5, 2s22p33s, 2s22p33d configurations has been examined. This dramatically reduces the excitation cross sections. The main contribution to the polarization potential is from the 2s2p5 state, the more so as Z increases.
As noted by Landman [3], there is significant singlet-triplet mixing within the 2s22p4 states for ions with higher Z. The introduction of this singlet-triplet mixing causes appreciable changes to the cross sections for ions Ca12+ and heavier. We also obtained the cross sections for the transitions 3P →1D, 1S.
To allow for finite densities, we have included plasma screening effects using the Debye-Hückel model as described by Zygelman and Dalgarno [4]. For the electric-quadrupole transitions considered here, plasma screening only becomes significant for small Debye lengths: for Fe18+ the screening cuts in for Λ < 10a0. This is consistent with work by other authors on hydrogenic ions [4,5].

References

[1] K. Alder, A. Winther Electromagnetic Excitation: Theory of Coulomb Excitation with Heavy Ions. North-Holland, Oxford (1975)
[2] R.S.I. Ryans et al Astron. Astrophys. 345,663 (1999)
[3] D.A. Landman, Astrophys. J. 240,709 (1980)
[4] B. Zygelman, A. Dalgarno, Phys. Rev. A 35,4085 (1987)
[5] K. Scheibner, J.C. Weisheit, N.F. Lane, Phys. Rev. A 35,1252 (1987)