Absolute dimensions of solar-type eclipsing binaries - II. V636 Centauri: A 1.05 primary with an active, cool, oversize 0.85 secondary

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Table 9:

Ages (Gyr) for the primary (p) and secondary (s) components of V636 Cen determined from comparison between their masses and radii and Claret models for different mixing length parameters and abundances.
	$[{\rm Fe/H}]$	$l/H_{\rm p}(p)$	$l/H_{\rm p}(s)$	Age(p)	Age(s)
1	-0.20	1.40	1.00	$1.33 \pm 0.13$	$1.37 \pm 0.55$
2	-0.20	1.50	1.10	$1.82 \pm 0.13$	$3.10 \pm 0.55$
3	-0.12	1.60	1.10	$2.46 \pm 0.12$	$3.25 \pm 0.53$
4	-0.20	1.68	1.68	$2.40 \pm 0.13$

Note: Ages in Gyr. Except for those with the solar $l/H_{\rm p} = 1.68$ (case 4), the models
fit the observed effective temperatures within errors. See text for details.

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