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*Astron. Astrophys. Suppl. Ser.* **135**, 347-357

## Atomic data from the Iron Project

### XXXV. Relativistic fine structure oscillator strengths
for Fe XXIV and Fe XXV

**S.N. Nahar and A.K. Pradhan**

**Send offprint request: **S.N. Nahar

Department of Astronomy, The Ohio State University,
Columbus, OH 43210, U.S.A.

Internet: nahar@astronomy.ohio-state.edu

Received August 27; accepted October 21, 1998

### Abstract:

The first large-scale calculations of relativistic radiative transition
probabilities from the Iron Project is reported for dipole allowed and
intercombination (E1) transitions in Li-like Fe XXIV and He-like Fe XXV. The
ab intio calculations are carried out in the close coupling approximation
using the Breit-Pauli R-matrix method in intermediate coupling
characterized by SLJ, with total (2*S*+1) = 2,4, *L* = 7, *J* = 1/2 - 11/2
even and odd parity, for Fe XXIV, and with total (2*S*+1) = 1,3, *L* = 9, and
*J* = 0 - 4 for Fe XXV. The eigenfunction expansions for the target ions
include 13 levels up to the *n*=3 for Fe XXV, and 16 levels up to the *n* = 4
for Fe XXVI, respectively. The calculated number of bound levels, 83
for Fe XXIV and 138 for Fe XXV, is much larger than experimentally
observed. The level energies are in good agreement for the common levels.
All dipole and intercombination fine structure transitions involving
the calculated bound levels up to *n* = 10 and = 5 or 6 are considered.
Oscillator strengths,
line strengths, and Einstein *A*-coefficients are tabulated for
802 transitions in Fe XXIV and 2579 transitions in Fe XXV.
The results compare well with
limited subsets of transitions considered in previous works including
fully relativistic and QED corrections.
Additional comparisons between
the length and the velocity formulations indicate an overall accuracy
between . The range of uncertainty is indicative of the
relatively small influence of atomic effects, such as the two-body
Breit interaction terms and finite nuclear
mass term, that are not included in the Breit-Pauli approximation
employed in the present calculations.
The extensive set of data is expected to be useful in
the analysis of X-ray and XUV spectra from astrophysical
sources^{}.

**Key words: ** atomic data -- X-ray: galaxies

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