J/ApJS/167/343 Plasma Recombination rate coefficients (Bryans+, 2006) ================================================================================ Collisional ionization equilibrium for optically thin plasmas. I. Updated recombination rate coefficients for bare through Sodium-like ions. Bryans P., Badnell N.R., Gorczyca T.W., Laming J.M., Mitthumsiri W., Savin D.W. =2006ApJS..167..343B ================================================================================ ADC_Keywords: Atomic physics Keywords: atomic data - atomic processes - plasmas Abstract: Reliably interpreting spectra from electron-ionized cosmic plasmas requires accurate ionization balance calculations for the plasma in question. However, much of the atomic data needed for these calculations have not been generated using modern theoretical methods and are often highly suspect. This translates directly into the reliability of the collisional ionization equilibrium (CIE) calculations. We make use of state-of-the-art calculations of dielectronic recombination (DR) rate coefficients for the hydrogenic through Na-like ions of all elements from He up to and including Zn. Where measurements exist, these published theoretical DR data agree with recent laboratory work to within typically 35% or better at the temperatures relevant for CIE. We also make use of state-of-the-art radiative recombination (RR) rate coefficient calculations for the bare through Na-like ions of all elements from H through to Zn. Here we present improved CIE calculations for temperatures from 104 to 109 K using our data and the recommended electron impact ionization data of Mazzotta et al. (1998, Cat. ) for elements up to and including Ni and Mazzotta (2000, private communication) for Cu and Zn. DR and RR data for ionization stages that have not been updated are also taken from these two additional sources. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table4.dat 224 1530 H - Zn Collisional Ionization Equilibrium (CIE) abundances (autostructure-based) table5.dat 211 357 Mg - Ni Collisional Ionization Equilibrium (CIE) abundances (FAC-based results) -------------------------------------------------------------------------------- See also: J/A+AS/133/403 : Ionization balance for optically thin plasmas (Mazzotta+ 1998) J/ApJS/167/334 : Radiative recombination data for plasmas (Badnell+, 2006) Byte-by-byte Description of file: table4.dat table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 A2 --- El Element 4- 7 F4.2 [K] logT [4/9] Log of the electron temperature 9- 14 F6.3 [-] Ab0 ? -Log of the fractional abundance for El (1) 16- 21 F6.3 [-] Ab1 ? -Log of the fractional abundance for El^1+^ (1) 23- 28 F6.3 [-] Ab2 ? -Log of the fractional abundance for El^2+^ (1) 30- 35 F6.3 [-] Ab3 ? -Log of the fractional abundance for El^3+^ (1) 37- 42 F6.3 [-] Ab4 ? -Log of the fractional abundance for El^4+^ (1) 44- 49 F6.3 [-] Ab5 ? -Log of the fractional abundance for El^5+^ (1) 51- 56 F6.3 [-] Ab6 ? -Log of the fractional abundance for El^6+^ (1) 58- 63 F6.3 [-] Ab7 ? -Log of the fractional abundance for El^7+^ (1) 65- 70 F6.3 [-] Ab8 ? -Log of the fractional abundance for El^8+^ (1) 72- 77 F6.3 [-] Ab9 ? -Log of the fractional abundance for El^9+^ (1) 79- 84 F6.3 [-] Ab10 ? -Log of the fractional abundance for El^10+^ (1) 86- 91 F6.3 [-] Ab11 ? -Log of the fractional abundance for El^11+^ (1) 93- 98 F6.3 [-] Ab12 ? -Log of the fractional abundance for El^12+^ (1) 100-105 F6.3 [-] Ab13 ? -Log of the fractional abundance for El^13+^ (1) 107-112 F6.3 [-] Ab14 ? -Log of the fractional abundance for El^14+^ (1) 114-119 F6.3 [-] Ab15 ? -Log of the fractional abundance for El^15+^ (1) 121-126 F6.3 [-] Ab16 ? -Log of the fractional abundance for El^16+^ (1) 128-133 F6.3 [-] Ab17 ? -Log of the fractional abundance for El^17+^ (1) 135-140 F6.3 [-] Ab18 ? -Log of the fractional abundance for El^18+^ (1) 142-147 F6.3 [-] Ab19 ? -Log of the fractional abundance for El^19+^ (1) 149-154 F6.3 [-] Ab20 ? -Log of the fractional abundance for El^20+^ (1) 156-161 F6.3 [-] Ab21 ? -Log of the fractional abundance for El^21+^ (1) 163-168 F6.3 [-] Ab22 ? -Log of the fractional abundance for El^22+^ (1) 170-175 F6.3 [-] Ab23 ? -Log of the fractional abundance for El^23+^ (1) 177-182 F6.3 [-] Ab24 ? -Log of the fractional abundance for El^24+^ (1) 184-189 F6.3 [-] Ab25 ? -Log of the fractional abundance for El^25+^ (1) 191-196 F6.3 [-] Ab26 ? -Log of the fractional abundance for El^26+^ (1) 198-203 F6.3 [-] Ab27 ? -Log of the fractional abundance for El^27+^ (1) 205-210 F6.3 [-] Ab28 ? -Log of the fractional abundance for El^28+^ (1) 212-217 F6.3 [-] Ab29 ? -Log of the fractional abundance for El^29+^ (1) 219-224 F6.3 [-] Ab30 ? -Log of the fractional abundance for El^30+^ (1) -------------------------------------------------------------------------------- Note (1): * For H we use the RR rate coefficients of Badnell (2006, Atomic and Molecular Diagnostic Processes in Plasmas, http://amdpp.phys.strath.ac.uk/tamoc/RR/ ) and EII rate coefficients of Mazzotta et al. (1998 Cat. ) * For He-Mg, same as H but also using the DR rate coefficients of Badnell (2006, Atomic and Molecular Diagnostic Processes in Plasmas, http://amdpp.phys.strath.ac.uk/tamoc/DR/ ). * For Al-Ni, same as He-Mg but also using the DR and RR rate coefficients of Mazzotta et al. (1998, Cat. ) for ions not calculated by Badnell (2006, http://amdpp.phys.strath.ac.uk/tamoc/RR/ and http://amdpp.phys.strath.ac.uk/tamoc/DR/ ) * For Cu-Zn, we use the DR rate coefficients of Badnell (2006, (http://amdpp.phys.strath.ac.uk/tamoc/RR/) for H-like through Na-like ions, RR rate coefficients of Badnell (2006, http://amdpp.phys.strath.ac.uk/tamoc/DR/) for bare through Na-like ions, DR and RR rate coefficients of Mazzotta (priv. com.) for all other ions, and the EII rate coefficients of Mazzotta (priv. com.). * For Mg we use the DR rate coefficients of Gu (2003ApJ...590.1131G, 2004ApJS..153..389G) for H-like through Na-like ions, RR rate coefficients of Gu (2003ApJ...589.1085G) for bare through F-like ions, RR rate coefficient of Mazzotta et al. (1998, ) for the Na-like ion, and EII rate coefficients of Mazzotta et al. (1998, ). * For Si-Ni, same as Mg but also using the DR and RR rate coefficients of Mazzotta et al. (1998, ) for ions not calculated by Gu (2003ApJ...589.1085G, 2003ApJ...590.1131G, 2004ApJS..153..389G) Fractional abundances are cut off at 10^-15^. For ease of machine readability, values less than 10^-15^ are given -log_10_ values of 15. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Greg Schwarz [AAS], Patricia Vannier [CDS] 29-May-2008