View
220
Download
0
Tags:
Embed Size (px)
Citation preview
Th
e C
HIA
NT
I d
atab
ase
Adding Ionization and Recombination to CHIANTI
Dr Peter YoungCCLRC/Rutherford Appleton Laboratory, UK
Dr Ken DereGeorge Mason University, USA
Th
e C
HIA
NT
I d
atab
ase
Th
e C
HIA
NT
I d
atab
ase
Background
• Tables of ion fractions as a function of temperature are essential for the analysis of electron-ionized plasmas
• In the past, rates have been re-assessed on timescales of ~5 years and new tables published
• Previous calculations include– Mazzotta et al. (1998)– Arnaud & Raymond (1992)– Arnaud & Rothenflug (1985)– Shull & Van Steenberg (1982)
Th
e C
HIA
NT
I d
atab
ase
CHIANTI
• CHIANTI contains atomic data for the calculation of level populations within ions
• Major updates occur every ≈ 2 years
• There is no official CHIANTI ion fraction data-set• The user can choose any of the standard ion fraction tables
Th
e C
HIA
NT
I d
atab
ase
CHIANTI version 6
• v.6 of CHIANTI will provide– ionization rates– recombination rates– ion fractions derived from these rates
Th
e C
HIA
NT
I d
atab
ase
Ionization
• Ionization rates have been assessed, and new calculations performed for many ions– K.P. Dere (2006, submitted to ApJ)
• Experimental cross-section data have been fit with a Burgess & Tully (1992) type fitting formula
• High energy limit given by the Bethe coefficient
f – scaling parameter; I – ionization potential; u = E/I; σ – cross-section
Th
e C
HIA
NT
I d
atab
ase
Fitting the rates
• The ionization rate coefficients are also fit with a Burgess-Tully type scaling
• The spline fits to these scaled rates will be provided to the CHIANTI user
f – scaling parameter; I – ionization potential; t = kT/I; σ – rate coefficient
Th
e C
HIA
NT
I d
atab
ase
Ionization: FAC calculations
• For many ions where experimental data are incomplete or missing, new data have been calculated
• The Flexible Atomic Code (FAC) has been used– relativistic distorted wave code similar to that of Zhang & Sampson
(1991)
Example: Ni XIV
Th
e C
HIA
NT
I d
atab
ase
Radiative Recombination
• The baseline set of radiative recombination rates are derived from fits embedded in a fortran routine of D.A. Verner
• Gives rates for all ions of all elements up to zinc
• These rates are used as the baseline, supplemented by– Badnell (2006)– Wane & Aymar (1987)– Aldrovandi & Pequignot (1974)
Th
e C
HIA
NT
I d
atab
ase
Radiative Recombination Problems
• Beyond the sodium sequence, most of the data have been obtained by interpolation/extrapolation of the Woods et al. (1981) data-set for the iron ions
• Comparisons with other data-sets show differences
Th
e C
HIA
NT
I d
atab
ase
Dielectronic recombination
• Baseline DR rates are taken from Mazzotta et al. (1998)
• New DR rates for all sequences up to the sodium sequence have been calculated by N.R. Badnell and co-workers
• Rates for Cu and Zn were not provided by Mazzotta et al. (1998). These are taken from Mazzitelli & Mattioli (ADNDT, 2002)
Th
e C
HIA
NT
I d
atab
ase
Comparison with Nahar data
• S. Nahar and colleagues have calculated combined RR and DR rates for many ions
• Significant differences exist for some ions for cases where new Badnell data are available, and also where older data are being used