Abstract
Neutral Chromium (Cr I) is an important element in many laboratory plasma applications. In this work, expectation values of the radius for Cr I are calculated. These atomic data are calculated with three different atomic codes: Cowan code using the Hartree–Fock Relativistic approximation, SUPERSTRUCTURE and AUTOSTRUCTURE codes using scaled Thomas–Fermi–Dirac–Amaldi potential. Relativistic corrections are introduced according to the Breit–Pauli approach. The 3 d 5 4 s , 3 d 4 4 s 2 , 3 d 5 4 d , 3 d 5 4 p and 3 d 4 4 s 4 p configurations are included to obtain the expectation values of radius of Cr I and compared with available data. The novelty of our work is to obtain new values of < 1 r > , < r > , and < r 2 > for the configuration of 4 p and 4 d and the values of < r 3 > for all orbitals configurations considered in this work.
Highlights
The Chromium (Cr I) is a transition metal and has electronic configuration as [Ar] 3d5 4s1, ground-state level: 7 S3 and ionization energy: 6.76651 eV (National Institute of Standards and Technology (NIST) database [1])
The radial integrals F k were kept at 85%, the exchange integral G k and configuration interaction integrals Rk were kept at 80% of the Hartree–Fock Relativistic (HFR) values
The values obtained by the three atomic structure codes are in good agreement in general, but hydrogen approximation (HA) gives good values only for the inner orbits
Summary
The Chromium (Cr I) is a transition metal and has electronic configuration as [Ar] 3d5 4s1 , ground-state level: 7 S3 and ionization energy: 6.76651 eV (National Institute of Standards and Technology (NIST) database [1]). Description and analysis of the first spectrum of neutral chromium (Cr I) have been studied experimentally by Kiss 1953 [2]. For laboratories and astrophysical plasmas, the study of chromium is important and it occurs in some fusion experiments. Many laboratory techniques are used to have Cr I atomic structure data (see Sobeck et al 2007 [3]). Chromium in its various ionization stages is important for analyzing atmospheres of some stars and many works are done for the chromium in astrophysical plasmas (see [4])
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