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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Volume 502 / No 1 (July IV 2009)

A&A, 502 1 (2009) 253-265

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Table 1:

Photometric solutions for V636 Cen from JKTEBOP analyses of the 1987 and 1988 light curve observations (426 points per band).
	y	b	v	u
i ( $^\circ$ )	89.65	89.62	89.62	89.63
	$\pm$ 7	$\pm$ 7	$\pm$ 8	$\pm 9$
$r_{\rm p}$	0.0746	0.0748	0.0750	0.0751
	$\pm$ 5	$\pm$ 5	$\pm$ 6	$\pm$ 6
$r_{\rm s}$	0.0613	0.0614	0.0613	0.0614
	$\pm$ 3	$\pm$ 3	$\pm$ 3	$\pm$ 3
k	0.822	0.822	0.818	0.817
	$\pm$ 5	$\pm$ 5	$\pm$ 6	$\pm$ 6
$r_p + r_{\rm s}$	0.1359	0.1362	0.1363	0.1365
	$\pm$ 6	$\pm$ 5	$\pm$ 7	$\pm$ 7
$u_{\rm p}$	0.59	0.68	0.77	0.81
$u_{\rm s}$	0.73	0.84	0.95	0.99
$y_{\rm p}$	0.37	0.43	0.49	0.58
$y_{\rm s}$	0.44	0.51	0.59	0.70
$J_{\rm s}/J_{\rm p}$	0.417	0.370	0.286	0.236
	$\pm$ 10	$\pm$ 9	$\pm$ 8	$\pm$ 7
$L_{\rm s}/L_{\rm p}$	0.265	0.233	0.176	0.144
	$\pm$ 3	$\pm$ 3	$\pm$ 3	$\pm$ 3
$\sigma$ (mmag.)	11.3	11.4	13.2	14.5

Note 1: Orbital parameters of e = 0.1348 and $\omega = 281\hbox{$.\!\!^\circ$ }60$ were assumed (Table 5), and linear limb darkening coefficients by Van Hamme (1993) were adopted.

Note 2: The errors quoted for the free parameters are realistic values determined from 1000 Monte Carlo simulations. e and $\omega$ were perturbed corresponding to their uncertainties, and the limb darkening coefficients within ${\pm} 0.05$ .

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