Access to Astronomical Catalogues

J/A+AS/119/99       [Ni I] & [Ni II] transition probabilities (Quinet+, 1996)
Transition probabilities for [Ni I] and [Ni II] lines.
     Quinet P., Le Dourneuf M.
    <Astron. Astrophys. Suppl. Ser. 119, 99 (1996)>
    =1996A&AS..119...99Q      (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics

Keywords: atomic data - Ni I - Ni II - transition probabilities


Description:
    New radiative transition probabilities have been calculated for
    forbidden lines of astrophysical interest in Ni I and Ni II. The
    accuracy of the transition probability scales is established on the
    basis of two independent calculations performed with the approximately
    relativistic Hartree-Fock (HFR) and SUPERSTRUCTURE (SST) codes. Both
    physical models take into account the most important configuration
    interaction (CI) and relativistic effects.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table7            54       53   Radiative transition probabilities, Aki in s-1,
                                 as obtained with HFR and SST for forbidden
                                 lines of Ni I.
table8            54      110   Radiative transition probabilities, Aki in s-1,
                                 as obtained with HFR and SST for forbidden
                                 lines of Ni II.


Byte-by-byte Description of file: table7

   Bytes Format  Units   Label      Explanations

   1-  8  A8     ---     Multiplet  Multiplet designation
   9- 11  A3     ---     J-J'       J-J'
  12- 22  F11.2  0.1nm   Lambda     Predicted wavelengths from observed
                                    energy levels: see note (1)
  23- 30  A8     ---     Type       Type of transition
  31- 41  E11.2  s-1     Aki(HFR)   HFR transition probabilities
      42  A1     ---    n_Aki(HFR)  [*] Comment on the HFR A-value: see note (2)
  43- 53  E11.2  s-1     Aki(SST)   SST transition probabilities

Note (1): Predicted wavelengths are deduced from the observed energy levels
           (Litzen et al. 1993). They are given in air above 200nm and in
           vacuum below 200nm.
Note (2): * Cancellation effects present.



Byte-by-byte Description of file: table8

   Bytes Format  Units   Label      Explanations

   1-  8  A8     ---     Multiplet  Multiplet designation
   9- 11  A3     ---     2J-2J'     2J-2J'
  12- 22  F11.2  0.1nm   Lambda     Predicted wavelengths from observed
                                     energy levels: see note (1)
      23  A1     ---     n_Lambda   [+] Comment on the wavelength: see note (2)
  24- 30  A7     ---     Type       Type of transition
  31- 41  E11.2  s-1     Aki(HFR)   HFR transition probabilities
      42  A1     ---    n_Aki(HFR)  [*] Comment on the HFR A-value: see note (3)
  43- 53  E11.2  s-1     Aki(SST)   SST transition probabilities

Note (1): Predicted wavelengths are deduced from the observed energy levels
          (Sugar and Corliss 1985). They are given in air above 200nm and in
          vacuum below 200nm.
Note (2): + Calculated HFR wavelength.

Note (3): * Cancellation effects present.



Courtesy: Pascal Quinet 


References:
    Litzen U., Brault J.W., Thorne A.P., 1993, Phys. Scr. 47, 628.
    Sugar J., Corliss C., 1985, J. Phys. Chem. Ref. Data 14, Suppl. 2
(End)                                         Patricia Bauer [CDS]   25-Mar-1996