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 2:

WD solutions from the 1987 light curve observations (165 per band).
	y	b	v	u
i ( $^\circ$ )	89.80	89.63	89.83	89.81
	$\pm$ 3	$\pm$ 2	$\pm$ 2	$\pm$ 4
$\Omega_{\rm p}$	14.504	14.465	14.395	14.397
	$\pm$ 22	$\pm$ 33	$\pm$ 38	$\pm$ 49
$\Omega_{\rm s}$	14.738	14.666	14.725	14.720
	$\pm$ 17	$\pm$ 34	$\pm$ 40	$\pm$ 56
$r_{\rm p}$ ^a	0.0737	0.0739	0.0743	0.0743
$r_{\rm s}$ ^a	0.0601	0.0604	0.0601	0.0602
k	0.815	0.817	0.809	0.810
$r_{\rm p} + r_{\rm s}$	0.1338	0.1343	0.1344	0.1345
$T_{\rm s}$ (K)	4965	4984	4916	4962
	$\pm$ 6	$\pm$ 5	$\pm$ 7	$\pm$ 7
$L_{\rm s}/L_{\rm p}$	0.286	0.256	0.199	0.172
LO₁ ( $^\circ$ )	12.2	15.0	17.2	31.8
	$\pm$ 3.7	$\pm$ 3.2	$\pm$ 3.3	$\pm$ 6.6
AR₁ ( $^\circ$ )	23.9	25.7	29.6	31.8
	$\pm$ 1.0	$\pm$ 0.8	$\pm$ 1.0	$\pm$ 1.2
LO₂ ( $^\circ$ )	233.0	235.3	233.8	255.6
	$\pm$ 7.6	$\pm$ 3.7	$\pm$ 3.5	$\pm$ 10.1
AR₂ ( $^\circ$ )	17.7	19.3	22.5	25.7
	$\pm$ 1.4	$\pm$ 0.8	$\pm$ 1.2	$\pm$ 1.2
$\sigma$ (mmag.)	6.2	6.2	7.7	9.1

^a Relative volume radius

Note 1: $T_{\rm p}$ was assumed to be 5900 K; for orbital parameters and limb darkening coefficients see Table 1.

Note 2: The errors quoted for the free parameters are the formal probable errors determined from the iterative least squares solution procedure.

Source LaTeX | All tables | In the text

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