Resolved Specific Ion Data Collections

Temperature Range
0.086 eV → 86.17 eV


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  • Spontaneous Emission: Ne+4(i) → Ne+4(j) + hv
  • Electron Impact Excitation: Ne+4(i) + e → Ne+4(j) + e
2s22p2(3p) 3P0.0 0.0 cm-1
2s22p2(3p) 3P1.0 412.0 cm-1
2s22p2(3p) 3P2.0 1110.0 cm-1
2s22p2(1d) 1D2.0 30291.0 cm-1
2s22p2(1s) 1S0.0 63914.0 cm-1
2s12p3(5s) 5S2.0 88360.0 cm-1
2s12p3(3d) 3D3.0 175834.0 cm-1
2s12p3(3d) 3D2.0 175905.0 cm-1
2s12p3(3d) 3D1.0 175926.0 cm-1
2s12p3(3p) 3P2.0 208157.0 cm-1
2s12p3(3p) 3P1.0 208158.0 cm-1
2s12p3(3p) 3P0.0 208193.0 cm-1
2s12p3(1d) 1D2.0 270564.0 cm-1
2s12p3(3s) 3S1.0 279365.0 cm-1
2s12p3(1p) 1P1.0 303812.0 cm-1
2p4(3p) 3P2.0 412681.0 cm-1
2p4(3p) 3P1.0 413466.0 cm-1
2p4(3p) 3P0.0 413803.0 cm-1
2p4(1d) 1D2.0 458113.0 cm-1
2p4(1s) 1S0.0 525541.0 cm-1
2s22p3s(3p) 3P0.0 596254.0 cm-1
2s22p3s(3p) 3P1.0 596626.0 cm-1
2s22p3s(3p) 3P2.0 597523.0 cm-1
2s22p3s(1p) 1P1.0 605231.0 cm-1
2s22p3p(1p) 1P1.0 635400.0 cm-1
2s22p3p(3d) 3D1.0 640422.0 cm-1
2s22p3p(3d) 3D2.0 640868.0 cm-1
2s22p3p(3d) 3D3.0 641646.0 cm-1
2s22p3p(3s) 3S1.0 646370.0 cm-1
2s22p3p(3p) 3P0.0 650699.0 cm-1
2s22p3p(3p) 3P1.0 651100.0 cm-1
2s22p3p(3p) 3P2.0 651600.0 cm-1
2s22p3p(1d) 1D2.0 663500.0 cm-1
2s22p3p(1s) 1S0.0 678500.0 cm-1
2s22p3d(3f) 3F2.0 690000.0 cm-1
2s22p3d(1d) 1D2.0 690691.0 cm-1
2s22p3d(3f) 3F3.0 690899.0 cm-1
2s22p3d(3f) 3F4.0 691500.0 cm-1
2s2p23s(5p) 5P1.0 697025.0 cm-1
2s2p23s(5p) 5P2.0 697577.0 cm-1
2s2p23s(5p) 5P3.0 698031.0 cm-1
2s22p3d(3d) 3D1.0 698231.0 cm-1
2s22p3d(3d) 3D2.0 698382.0 cm-1
2s22p3d(3d) 3D3.0 698735.0 cm-1
2s22p3d(3p) 3P2.0 701765.0 cm-1
2s22p3d(3p) 3P1.0 702074.0 cm-1
2s22p3d(1p) 1P1.0 702412.0 cm-1
2s22p3d(3p) 3P0.0 702459.0 cm-1
2s22p3d(1f) 1F3.0 709956.0 cm-1

      Last updated October 22, 2001

      See: D C Griffin and N R Badnell 2000 J. Phys. B 33 4389 for a
      more complete description.


      From a 66-term 138-level Intermediate-Coupling Frame Transformation
      (ICFT) R-matrix calculation that included all levels of the
      configurations 2s22p2, 2p4, 2s2p3, 2s22p3s, 2s22p3p, 2s22p3d, and
      2s2p23s, 2s22p4s, 2s23p4p, 2s22p4d; and all the levels in 2s2p23p and
      2s2p23d that lie below the highest level of 2s22p4d.  In addition the
      remaining levels of 2s2p23p and 2s2p23d and all the levels of 2p33s,
      2p33p, and 2p33d were included in the CI expansion.  The 1s, 2s, and
      2p orbitals were determined from a single-configuration Hartree-Fock
      calculation on 2s22p2 3P.  The 3s, 3p, and 3d orbitals were
      determined from multi-configuration Hartree-Fock calculations on
      2s22p3s+2P33s 3P, 2s22p3p+2p33p 3D, and 2s22p3d+2p33d 3F,
      respectively, and the 4s, 4p, and 4d orbitals were determined from
      single-configuration Hartree-Fock calculations on 1s22p4l.  In STG3
      of the R-matrix calculation, the term energies were adjusted to the
      experimental term energies and in the ICFT calculation, the level
      energies were adjusted to the experimental values where known.

      For the JPI partial waves from J=0.5 to 9.5 and even and odd parity,
      we performed an LS R-matrix calculation with exchange for the LSPI
      partial waves with L = 0 to L = 12 and then transformed the
      unphysical K-matrices to intermediate coupling using the ICFT method.
      For the higher partial waves, we performed a no-exchange calculation
      in LS coupling, with the long-range multipoles included, for all LSPI
      partial waves from L = 8 to 40; transformed the unphysical K-matrices
      to intermediate-coupling; and topped up.  This allowed us to add the
      partial-wave contributions from J = 10.5 to 37.5.  The size of
      the continuum basis for these calculations was set to 24.  The number
      of mesh points used in the asymptotic part of the problem was 8740
      and the maximum energy was 15 Ry.

      The radiative rates for the dipole-allowed transitions were
      determined from our 261-level CI calculation in the Breit-Pauli

      The numbers in the last column of the above table are the theoretical
      values for the reduced effective collision strengths in the infinite
      temperature limit as defined in Burgess and Tully Astron. Astrophys.
      254 436 (1992).

                                        Donald C. Griffin

      D Griffin extended the data to lower temperatures and added the limit
      points. This file replaces the original version.

      Martin O'Mullane

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