Updated Coronal Equilibrium Calculations

Details Updated Coronal Equilibrium Calculations Updated Coronal Equilibrium Calculations

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0101b&link_type=abstract

American Astronomical Society, SPD meeting #37, #1.01; Bulletin of the American Astronomical Society, Vol. 38, p.215

Astronomy and Astrophysics

Astronomy

Scientific paper

Reliably interpreting solar spectra requires accurate ionization balance calculations. 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 through to Zn. We also make use of state-of-the-art radiative recombination (RR) rate coefficient calculations for the bar e through Na-like ions of all elements from H to Zn. Here we present improved CIE calculations for temperatures from 1e4 to 1e9 K using our data and the recommended electron impact ionization data of Mazzotta et al. (1998, A&AS, 133, 403) for elements up through Ni and Mazzotta (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. We compare our calculated fractional ionic abundances using these data with those presented by Mazzotta et al. for all elements from H to Ni. The differences in peak fractional abundance are up to 60%. We also compare with the fractional ionic abundances for Mg, Si, S, Ar, Ca, Fe, and Ni derived from the modern DR calculations of Gu (2003a, ApJ, 590, 1131; 2004, ApJ, 153, 389) for the H-like through Na-like ions, and the RR calculations of Gu (2003b, ApJ, 589, 1085) for the bare through F-like ions. These results are in better agreement with our work, with differences in peak fractional abundance of less than 10%.
This work was supported in part by the NASA Solar SR&T and LWS programs, theOffice of Naval Research, and PPARC.

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