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We studied the dielectronic recombination processe of Ni17+(3s) through the resonant doubly excited states Ni16+(3pnl,3dnl) (Δn=0) using the Flexible Atomic Code (FAC) which is based on a relativistic configuration interaction method. We obtained the cross sections and the rate coefficients and compared them with the experimental data and other theoretical results. The integrated cross sections through the resonant doubly excited states 3p3/210l and 3p1/211l are in a good agreement with the measurements within the experimental errors. In combination with quantum defect theory, we have found out that the radiative rates and the auger rates of the resonant doubly excited states involving high Rydberg states obey a good scaling law, by means of which we obtained the integrated cross sections and the rate coefficients of all the resonances close to the thresholds. A comparison of the series 3pnl and 3dnl indicates that the rate coefficients of the former are larger when the temperature is below ~100 eV, and are smaller when the temperature is higher.
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Keywords:
- dielectronic recombination /
- FAC code /
- quantum defect theory /
- rate coefficient
[1] Zong W, Schuch R, Lindroth E, Gao H, DeWitt D R 1997 Phys. Rev. A 56 386
[2] Glans P, Lindroth E, Badnell N R, Eklow N, Zong W, E Justiniano, Schuch R 2001 Phys. Rev. A 64 043609
[3] Tokman M, Eklow N, Glans P, Lindroth E, Schuch R 2002 Phys. Rev. A 66 012703
[4] Fogle M, Eklow N, Lindroth E, Mohamed T, Schuch R, Tokman M 2003 J. Phys. B: At. Mol. Opt. Phys. 36 2563
[5] Gu M F 2003 Astrophy. J. 582 1241
[6] Gu M F 2003 Astrophy. J 589 1085
[7] Gu M F 2003 Astrophy. J 590 1131
[8] Wang J G, Zou Y, Chang T Q 1997 Acta Phys. Sin. 46 11 (in Chinese) [王建国、邹 宇、常铁强 1997 46 11]
[9] Shi W, Bartsch T, Bohme C, Brandau C, Hoffknecht A, Knopp H, Schippers S 2002 Phys. Rev. A 66 22718.
[10] Andersen L H, Pan G Y, Schmidt H T 1992 Phys. Rev. A 45 7868.
[11] Kilgus G, Habs D, Schwalm D, Wolf A 1992 Phys. Rev. A 46 5730
[12] Wang J G, Tong X M, Li J M 1996 Acta Phys. Sin. 45 1 (in Chinese) [王建国、仝晓民、李家明 1996 45 1]
[13] Wang J G, Takako Kato, Izumi Murakami 1999 Phys. Rev. A 60 2104, 3750
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[1] Zong W, Schuch R, Lindroth E, Gao H, DeWitt D R 1997 Phys. Rev. A 56 386
[2] Glans P, Lindroth E, Badnell N R, Eklow N, Zong W, E Justiniano, Schuch R 2001 Phys. Rev. A 64 043609
[3] Tokman M, Eklow N, Glans P, Lindroth E, Schuch R 2002 Phys. Rev. A 66 012703
[4] Fogle M, Eklow N, Lindroth E, Mohamed T, Schuch R, Tokman M 2003 J. Phys. B: At. Mol. Opt. Phys. 36 2563
[5] Gu M F 2003 Astrophy. J. 582 1241
[6] Gu M F 2003 Astrophy. J 589 1085
[7] Gu M F 2003 Astrophy. J 590 1131
[8] Wang J G, Zou Y, Chang T Q 1997 Acta Phys. Sin. 46 11 (in Chinese) [王建国、邹 宇、常铁强 1997 46 11]
[9] Shi W, Bartsch T, Bohme C, Brandau C, Hoffknecht A, Knopp H, Schippers S 2002 Phys. Rev. A 66 22718.
[10] Andersen L H, Pan G Y, Schmidt H T 1992 Phys. Rev. A 45 7868.
[11] Kilgus G, Habs D, Schwalm D, Wolf A 1992 Phys. Rev. A 46 5730
[12] Wang J G, Tong X M, Li J M 1996 Acta Phys. Sin. 45 1 (in Chinese) [王建国、仝晓民、李家明 1996 45 1]
[13] Wang J G, Takako Kato, Izumi Murakami 1999 Phys. Rev. A 60 2104, 3750
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