Table 13: Photometric solutions for VZ Hya from the WD code adopting linear limb darkening coefficients by van Hamme (1993); see Table 12. 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.
  y b v u
i   ($^\circ$) 88.90 88.92 88.95 88.98
  $\pm$2 $\pm$1 $\pm$2 $\pm$2

$\Omega_{\rm p}$

 9.649 9.666 9.639 9.668
  $\pm$8 $\pm$7 $\pm$8 $\pm$11

$\Omega_{\rm s}$

 10.349 10.329 10.355 10.343
  $\pm$8 $\pm$7 $\pm$8 $\pm$11

$r_{\rm p}$

 0.1144 0.1142 0.1146 0.1142

$r_{\rm s}$

 0.0969 0.0971 0.0968 0.0969

k

 0.847 0.850 0.845 0.849

$r_{\rm p} + r_{\rm s}$

 0.2113 0.2113 0.2114 0.2111

$T_{\rm {eff},s}$

 6272 6252 6229 6182
  $\pm$2 $\pm$1 $\pm$2 $\pm$3

$L_{\rm s}/L_{\rm p}$

 0.5686 0.5464 0.5125 0.5347

$\sigma$   (mag.)

 0.0046 0.0039 0.0043 0.0068


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