Table 1: Experimental data for planets in binary systems. The last column is the mass (calculated with 6) for each star of a hypothetical binary system which would cause in the target star the same wobble as the planet (see text). Data taken from Eggenberger et al. (2004) and from the Extrasolar Planets Encyclopaedia (http://www.obspm.fr/planets).
Name $a_{\rm A} {\rm (AU)}$a $a_{\rm pl} {\rm (AU)}$b $M_{\rm pl}~(M_{J})$c $M~(M_{\odot})$d
HD 40979 6400 0.811 3.32 $3.0\times10^{7}$
GL 777 A 3000 4.8 1.33 $3.6\times10^{4}$
HD 80606 1200 0.469 3.90 $2.0\times10^{6}$
55 Cnc 1065 0.115 0.84 $1.8\times10^{7}$
    0.24 0.21 $1.4\times10^{6}$
    5.9 4.05 $3.7\times10^{3}$
16 Cyg B 850 1.6 1.5 $2.8\times10^{4}$
$\upsilon$ And 750 0.83 2.11 $1.3\times10^{5}$
    2.50 4.61 $1.5\times10^{4}$
HD 178911 B 640 0.32 6.292 $1.6\times10^{6}$
$\tau$ Boo 240 0.05 4.08 $1.1\times10^{7}$
HD 195019 150 0.14 3.51 $2.5\times10^{5}$
HD 114762 130 0.35 11.03 $3.9\times10^{4}$
HD 19994 100 1.33 1.78 $2.1\times10^{2}$
$\gamma$ Ceph 22 2.03 1.59 $1.9\times10^{0}$
Gl 86 20 0.11 4.0 $3.5\times10^{3}$
a Semimajor axis of the orbit of the binary stellar system in AU.
b Semimajor axis of the orbit of the planet in AU.
c Mass of the planet in Jupiter masses.
d Mass calculated with 6 for each star of the hypothetical binary system
  which would imitate the wobble of a planet.


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