55 Cnc 55 Cnc
(HD 75732) contains a star of late spectral type G or early type K, K0 IV-V (Gray et al. 2003) and five planets. The host star has effective temperature equal to 5196 ± 24 K, log g = 4.45 ± 0.01 (von Braun et al. 2011) and metallicity [Fe/H] = 0.31 ± 0.04 (Fischer and Valenti 2005). The mass and radius of the star are 0.905 ± 0.015 M ⊙ and 0.943 ± 0.010 R ⊙ respectively. The age of the star is evaluated to be 10.2 ± 2.5 × 109 years (von Braun et al. 2011). The dominant external planet is a gas giant with a minimal mass equal to 4 m J located at a distance of 5.8 AU from the star. Inside the gas giant orbit there are four less massive PF-02341066 clinical trial planets. The eccentricities of their orbits are very small, comparable to the eccentricities of the planets in the Solar System. The ratio of the orbital periods of planets b and c is 3.027 (Fischer et al. 2008), which might indicate the existence of the 3:1 mean-motion resonance. HD 60532 HD 60532 has a completely different structure from that of 55 Cnc, as it contains two very massive gas giants close to the 3:1 resonance.
The central star of this system is of spectral type F6 IV-V with effective temperature 6095 K, log(g) = − 3.83, and metallicity [Fe/H] = − 0.26. The mass of the star is 1.44 M ⊙ , while its estimated age is equal to 2.7 ± 0.1 × 109 years. The distance from the Sun is 25.7 pc. Laskar and Correia (2009) Etomoxir have confirmed the existence of the 3:1 commensurability using the global dynamical analysis of the system. They have obtained the best fit for the resonance configuration and for their best fit they have got the stability of the system for at least 5 × 109 years. In Table 1 the parameters
of the system are given for the inclination angle i ≈ 20 o . Sandor and Kley (2010) have presented one of the possible scenarios for the formation of this system, which is in the very good agreement with the observational data. υ And Very recently, it has been suggested that there is the 3:1 resonance in the system υ And. υ And was the first multi-planet extrasolar system discovered with the central star being a main sequence star (Butler DNA ligase et al. 1999). It is a bright star of spectral type F8V with mass 1.3 M ⊙ and radius 1.56 R ⊙ (Butler et al. 1999). Its distance from the Sun is 13.47 pc (Perryman et al. 1997). The age of the star is 5 × 109 years (Baliunas et al. 1997). The system contains four planets plus the newly discovered υ And e (Curiel et al. 2011). In this system there is just a 3:1 resonance formed by this DMXAA concentration recently found planet and planet d (Chavez et al. 2011). The stability analysis performed by Chavez et al. (2011) confirmed the existence of this 3:1 commensurability and indicated the stability of its structure in timescales of the order of 5 × 108 years. Now it is a turn for the 4:1 resonance, a third order commensurability.