2005 36th Meeting of the Division of Atomic, Molecular and Optical Physics
Tuesday–Saturday, May 17–21, 2005;
Lincoln, Nebraska
Session D6: Poster Session I
4:00 PM,
Wednesday, May 18, 2005
Burnham Yates Conference Center
Room: Lancaster 4:00-6:00 pm
Abstract ID: BAPS.2005.DAMOP.D6.116
Abstract: D6.00116 : Evolution of the L satellites in the X-ray emission spectra of $\beta $ region
Preview Abstract
Abstract
Author:
Surendra Poonia
(Division of Natural Resources and Environment, Central Arid Zone Research Institute, India)
The X-ray satellites L$\beta _{1}^{I}$, L$\beta _{1}^{II}$, L$\beta
_{1}^{III}$, L$\beta _{1}^{IV}$, L$\beta _{2}^{I}$, L$\beta
_{2}^{(b)}$, L$\beta _{2}^{II }$and L$\beta _{2}^{(c)}$ observed
in the L-emission spectra in elements with Z = 26 to 92, have been
calculated. The energies of various transitions have been
calculated by
available Hartree-Fock-Slater (HFS) data using the semi-empirical
Auger
transition energies in the doubly ionized atoms and their relative
intensities have been estimated by considering cross - sections
of singly
ionized 2x$^{-1}$ (x $\equiv $ s, p) states and then of subsequent
Coster-Kronig and shake off processes. The calculated spectra
have been
compared with the measured satellite energies in the L emission
spectra.
Their intense peaks have been identified as the observed
satellite lines.
The one to one correspondence between the peaks in calculated
spectra and
the satellites in measured spectra has been established on the
basis of the
agreement between the separations in the peak energies and those
in the
measured satellite energies. Group of transitions under the
transition
schemes L$_{2}$M$_{x}$-M$_{x}$M$_{4,5}$ and$_{
}$L$_{3}$M$_{x}$-M$_{x}$N$_{4,5}$ (x $\equiv $ 1-5), which give,
rise to
these satellites have been identified. It is observed that the
satellite
L$\beta _{2}^{(b)}$ in all these spectra can be assigned to the
superposition of $^{3}$F$_{4}-^{3}$G$_{5}$ and
$^{3}$F$_{4}-^{3}$D$_{3
}$transitions and that this must be most intense one out of all
these
satellites, contributing in order of decreasing intensity. Each
of the
remaining satellites is found to have different origin in different
elements. The possible contributions of the suitable transitions
to all
these lines have also been discussed.
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References:\newline
1. Y. Cauchois and C. Senemaud, X-Ray Wavelength Tables, 2$^{nd}$
ed., (Oxford: Pergamon) pp. 217-314, (1978).\newline
2. S.N.Soni, J. Phys. B: At. Mol. Opt. Phys. \textbf{23},
1117-1128, (1990).\newline
3. S. N. Soni and M. H. Massoud, J. Phys. Chem. Solids
\textbf{58(1)}, 145-151 (1997).\newline
4. S. N. Soni and S. Poonia, J. Phys. Chem. Solids
\textbf{61(9)}, 1509-1518 (2000).\newline
5. S. Poonia and S. N. Soni, J. Phys. Chem. Solids
\textbf{62(3)}, 503-511 (2001).
To cite this abstract, use the following reference: http://meetings.aps.org/link/BAPS.2005.DAMOP.D6.116