Table 1: Parameters of close-in extrasolar giant planets and their host stars with circular orbits with semi major axis <0.06 AU (as of June 2004).
Parameter     OGLE-TR 56 OGLE-TR 3 OGLE-TR-113 OGLE-TR 10 OGLE-TR 132
Spectral type     G0 G0 K G0 F
Planetary mass [$M_{\rm J}$]   1.450 0.500 1.35 0.700 1.010
Semi major axis [AU]   0.023 0.023 0.023 0.042 0.0306
revolution period [days]   1.212 1.190 1.43 3.101 1.690
Orbit excentricity     0.000 0.000 0.000 0.000 0.000
Stellar rotation [days]   18.399 27.757a 27.757a 27.757a 27.757a
Stellar mass [$M_{\odot}$]   1.040b 1.000b 0.770b 1.000b 1.340b
Stellar radius [$R_{\odot}$]   1.100b 1.106b 0.822b 1.106b $1.489{{\rm b}}$
    average 1.230 0.870 1.080d 1.300d 1.150d
Planetary ${\rm radius}^{{c}}$ [$R_{\rm J}$] maximum 1.972 1.383      
    minimum 0.861 0.604      
Roche zone [$R_{\odot}$]   2.706 2.721 2.022 2.721 3.663
Stellar J2 [10-6]   -2.749 -1.277 -0.681 -1.277 -2.325
I*     0.07 0.07 0.07 0.07 0.07
k2*     0.168 0.168 0.168 0.168 0.168
System property factor [ $ 10^{-3}~M_{\odot}^{\frac {1}{2}}~R_{\odot}^5$]   2.290 0.827 0.577 1.158 6.386
               
Parameter     OGLE-TR 58 BD-10 3166 HD 209458 HD 76700 HD 49674
Spectral type     G0 G4 G0 G6 G5
Planetary mass [$M_{\rm J}$]   1.600 0.480 0.690 0.197 0.120
Semi major axis [AU]   0.052 0.046 0.045 0.049 0.057
revolution period [days]   4.345 3.487 3.525 3.971 4.948
Orbit excentricity     0.000 0.000 0.000 0.000 0.000
Stellar rotation [days]   27.757a 27.757a 15.700 27.757a 27.757a
Stellar mass [ $M_{*{\odot}}$]   0.990b 1.100b 1.050b 1.000b 1.000b
Stellar radius [$R_{\odot}$]   1.106b 1.006b 1.200b 0.956b 0.981b
    average 1.600d 0.850 0.970 0.632 0.535
Planetary ${\rm radius}^{{c}}$ [$R_{\rm J}$] maximum   1.349 1.540 1.003 0.850
    minimum   0.589 0.673 0.438 0.371
Roche zone [$R_{\odot}$]   2.721 2.475 2.952 2.352 2.414
Stellar J2 [10-6]   -1.290 -0.874 -4.855 -0.825 -0.892
I*     0.07 0.07 0.07 0.07 0.07
k2*     0.168 0.168 0.168 0.168 0.168
System property factor [ $ 10^{-3}~M_{\odot}^{\frac {1}{2}}~R_{\odot}^5$]   2.661 0.472 1.676 0.157 0.109
a
If the true stellar rotation period is not known, the value was set, without loss of generality, to the sun's rotation period.
b
Derived from Aller et al. (1982).
c
If the planetary radius is not known, then upper and lower limits can be derived by setting the planetary bulk density to $250~{{\rm kg}}/{{\rm m}^3}$ (Henry et al. 2000; Jha et al. 2000) and $3000~{{\rm kg}}/{{\rm m}^3}$ (Cameron et al. 1999), respectively. As an average, the density of $1000~{{\rm kg}}/{{\rm m}^3}$ was assumed.
d
This is the true radius as derived from transit observations (Charbonneau et al. 2000; Konacki et al. 2003b).


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