The natural questions arising at this point are how such configurations Mocetinostat mouse were formed and do they carry some inPXD101 formation about the early stages of the evolution of our Solar System? The same questions become even more intriguing after the discovery of extrasolar planetary systems. Most mean-motion resonances are observed in systems containing gas giants (Table 1 in Section “Extrasolar Planets Close to Mean-Motion Resonances”), selleck however similar configurations can exist also in systems with low-mass planets. One example is that of the resonance 5:4 in the system Kepler-11
(Lissauer et al. 2011a). The reconstruction of the history of the planetary system formation may be possible thanks to the resonance phenomenon. That is why, it is so important to understand the process of the formation of the mean-motion resonances in the early stages of the planetary system evolution. Table 1 The planetary systems in which planets are in or close to the mean-motion resonance Object m p (m J ) a p (AU) Literature Kepler-11 b 0.0135 0.091 Lissauer et al. (2011a) c 0.0425 0.106 5:4 d 0.0192 0.159 e 0.0264 0.194 f 0.0072 0.250 g? <0.95 0.462 5:2 HD 200964 b 1.85 1.601 Johnson et al. (2011) c 0.90 1.95 4:3 PSR B1257+12 A 6 × 10 − 5 0.18850 Goździewski et al. (2005) B 0.013 0.35952 C 0.012 0.46604 3:2 HD 45364 b 0.1872 0.6813 Correia et al. (2009) c 0.6579 0.8972 3:2 Wasp-10 b 2.96 0.0369 Christian et al. (2009), Maciejewski et al.
(2011) c? 0.1 0.0536 5:3 Kepler-18 b 0.0217 0.0447 Cochran et al. (2011) c 0.054 0.0752 d 0.052 0.1172 2:1 HD 90043 (24 Sex) b 1.99 1.333 Johnson et al. (2011) c 0.86 2.08 2:1 HR 8799 e 7-10 14.5 Goździewski and Migaszewski Vorinostat in vivo (2009), Marois et al. (2010) d 7-10(8.891) 24(24.181) c 7-10(11.87) 38(39.646) 1:2:4 b 5-7(8.022) 68(68.448) HD 73526 b 2.9 0.66 Tinney et al. (2006) c 2.5 1.05 2:1 HD 82943 c 1.703 0.745 Beauge et al. (2008) b 1.747 1.200 4:2:1 d? 0.351 1.912 Wasp-3 b 2.06 0.0317 Maciejewski et al. (2010) c? 0.0472 0.0507 2:1 HD 128311 b 2.18 1.099 Goździewski and Konacki (2006) c 3.21 1.76 2:1 GJ 876 d 0.0221 0.0208 Baluev (2011) c 0.750 0.12959 b 2.39 0.20832 1:2:4 e 0.051 0.3343 Kepler-9 d? 0.022 0.0273 Holman et al. (2010) b 0.252 0.140 c 0.171 0.225 2:1 HD 160691 (μAra) d 0.032 0.09286 Goździewski et al. (2007) e 0.480 0.934 b 1.677 1.535 2:1 c 2.423 5.543 HD 37124 (Hip 26381) b 0.675 0.53364 Wright et al.