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Table 3:

Photometric solutions for V1130 Tau.
  y b v u
i ($^\circ$) 73.97 73.84 73.73 74.20
  $\pm $2 $\pm $4 $\pm $4 $\pm $6
$\Omega_{\rm p}$ 4.5138 4.5079 4.4954 4.5642
  $\pm $39 $\pm $40 $\pm $41 $\pm $64
$\Omega_{\rm s}$ 4.0727 4.0753 4.0775 4.0805
  $\pm $25 $\pm $29 $\pm $30 $\pm $45
$r_{\rm p}$ 0.2956 0.2961 0.2973 0.2911
$r_{\rm s}$ 0.3542 0.3539 0.3536 0.3532
k 1.198 1.195 1.189 1.213
$r_{\rm p} + r_{\rm s}$ 0.6498 0.6500 0.6509 0.6443
$u_{\rm p} = u_{\rm s}$ 0.52 0.61 0.67 0.63
$T_{{\rm eff},\rm s}$ 6638 6639 6643 6628
  $\pm $4 $\pm $3 $\pm $3 $\pm $4
$L_{\rm s}/L_{\rm p}$ 1.444 1.436 1.429 1.436
$\sigma$(mmag) 4.5 4.3 4.3 6.5

Notes. Limb darkening coefficients by van Hamme (1993), gravity darkening exponents of 0.33, and bolometric albedo coefficients of 0.5 were adopted, as appropriate for convective envelopes. $T_{{\rm eff},p}$was assumed to be 6650 K, see Sect. 6. The errors quoted for the free parameters are the formal standard errors determined from the iterative least squares solution procedure.


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