V945 Centauri = HD 112409: a bright hot short-period binary in a triple system?

P. Harmanec; C. Aerts; A. Prša; T. Verhoelst; K. Kolenberg

doi:10.1051/0004-6361/201014096

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Volume 520 (September-October 2010)

A&A, 520 (2010) A73

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Table 5:

Probable V945 Cen model parameters and their formal error estimates, where $\Omega$ is the value of the Roche-model potential used in the WD program, and L_i are the relative luminosities of the components in individual photometric passbands.
		Solution in the absence of 3rd light:			Solution in the presence of 3rd light:
Parameter:		Primary		Secondary	Primary		Secondary
a	$(R_{\hbox{$\odot$ }})$		$5.86 \pm 0.21$			$5.63 \pm 0.18$
i	$({}^\circ)$		23.0^*			24.0^*
$\Omega$		$3.625 \pm 0.018$		$3.695 \pm 0.012$	$3.496 \pm 0.024$		$3.608 \pm 0.015$
$T_{\rm eff}$	(K)	13000^*		$10930 \pm 40$	13000^*		$10687 \pm 52$
M	( $M_{\hbox{$\odot$ }}$ )	$3.74 \pm 0.58$		$2.67 \pm 0.54$	$3.32 \pm 0.51$		$2.37 \pm 0.48$
R	( $R_{\hbox{$\odot$ }}$ )	$2.20 \pm 0.09$		$1.73 \pm 0.07$	$2.09 \pm 0.12$		$1.67 \pm 0.09$
L	( $L_{\hbox{$\odot$ }}$ )	$123 \pm 20$		$35 \pm 6$	$111 \pm 21$		$37 \pm 7$
$M_{\rm bol}$	(mag)	$-0.50 \pm 0.2$		$0.87 \pm 0.2$	$-0.38 \pm 0.2$		$0.95 \pm 0.2$
$\log g$	[cgs]	$4.3 \pm 0.1$		$4.4 \pm 0.1$	$4.3 \pm 0.1$		$4.4 \pm 0.1$
L_i	B band	0.684		0.316	0.534	0.227	0.239
L_i	B1 band	0.688		0.312	0.536	0.223	0.241
L_i	B2 band	0.679		0.321	0.530	0.232	0.238
L_i	G band	0.667		0.333	0.517	0.242	0.242
L_i	U band	0.749		0.251	0.620	0.184	0.197
L_i	V band	0.669		0.331	0.519	0.240	0.241
L_i	V1 band	0.670		0.330	0.520	0.240	0.240
L_i	Hp band	0.679		0.321	0.529	0.232	0.239

Notes. They are normalized in such a way that L₁+L₂=1 for the first model without the third light, and L₁+L₂+L₃=1 for the triple-star model. Note that for this model, the values of L₃ are tabulated in the central column between the primary and secondary.
^* Values denoted with an asterisk are fixed.

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