Measurement of iron L-shell dielectronic recombination (DR) rates for X-ray photoionized nebulae: Fe XVIII and Fe XIX Δ n=0 DR

Details Measurement of iron L-shell dielectronic recombination (DR) rates for X-ray photoionized nebulae: Fe XVIII and Fe XIX Δ n=0 DR Measurement of iron L-shell dielectronic recombination (DR) rates for X-ray photoionized nebulae: Fe XVIII and Fe XIX Δ n=0 DR

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aps..apr.d1557s&link_type=abstract

American Physical Society, APS/AAPT Joint Meeting, April 18-21, 1997, abstract #D15.57

Astronomy and Astrophysics

Astronomy

Scientific paper

In an X-ray photoionized nebula (XPN) the ionization structure is driven by photoionization balanced by radiative recombination (RR) and DR; and the electron temperature at which an ion is formed is far below the temperature at which the ion would exist in coronal equilibrium. (Kallman et al.), Astrophys. J. 465, 994 (1996). (Arnaud, M. and Raymond, J., Astrophys. J. 398), 394 (1992). As a result of the low electron temperature in an XPN, X-ray line emission is produced by RR and DR and not by electron impact excitation.^ 1 For the iron L-shell ions (Fe XVII to Fe XXIV) which are a dominant source of line emission in the 0.8-2.0 keV bandpass, DR proceeds via Δ n=0 core excitations. To address the needs for interpreting spectra from present and upcoming X-ray astronomy satellite missions, we have initiated a program to measure the Δ n=0 DR rate coefficients for the iron L-shell ions. We will present our first results on DR of Fe XVIII and Fe XIX.

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