Fine-structure infrared lines from the Cassiopeia A knots

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Volume 509 (January 2010)

A&A, 509 (2010) A59

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Table 7:

Estimated FMK post-shock cooling region ionic abundances $n_{\rm ion}/n_{\rm O}$ . (See text for details).
Line	I/I(5007 Å)	$T_{\rm e}$ , K	$\varepsilon$ , cm³/s	$\Delta t$ , 10³ s	$n_{\rm ion}/n_{\rm O}$	$n_{\rm ion}/n_{\rm O}$ (model)^*
[Si X] 1.430 $\mu$ m	0.0016	$2\times10^4$	$2.9\times10^{-8}$	40	$7\times10^{-5}$	$5\times10^{-4}$
[Si VI] 1.964 $\mu$ m	0.004	$1\times10^4$	$3.1\times10^{-9}$	40	0.002	0.01
[Mg V] 5.608 $\mu$ m	<0.003	$6\times10^3$	$9.0\times10^{-9}$	30	<0.002	$4\times10^{-4}$
[Ar V] 7.914 $\mu$ m	0.005^**	$1\times10^4$	$1.3\times10^{-8}$	60	$8\times10^{-4}$	$5\times10^{-5}$
[Ne V] 14.32 $\mu$ m	0.015	$1\times10^4$	$2.4\times10^{-9}$	50	0.06	0.002

^* Estimated based on SD-200 model. The elemental abundances assumed to deduce the model ionic abundances with respect to oxygen are given in Table 9; ^** this line is partly arising in the pre-shock region. As follows from Table 6, the post-shock region contribution is I/I(5007 Å $)\approx0.0025$ .

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