We report the detection of planets around two evolved giant stars from radial velocity measurements at Okayama Astrophysical observatory .
24 Boo ( G3IV ) has a mass of 0.99 M _ { \Sol } , a radius of 10.64 R _ { \Sol } , and a metallicity of { [ Fe / H ] } = -0.77 .
The star hosts one planet with a minimum mass of 0.91 M _ { Jup } and an orbital period of 30.35 \ > { d } .
The planet has one of the shortest orbital periods among those ever found around evolved stars by radial-veloocity methods .
The stellar radial velocities show additional periodicity with 150 \ > { d } , which are probably attributed to stellar activity .
The star is one of the lowest-metallicity stars orbited by planets currently known . \gamma Lib ( K0III ) is also a metal-poor giant with a mass of 1.47 M _ { \Sol } , a radius of 11.1 R _ { \Sol } , and { [ Fe / H ] } = -0.30 .
The star hosts two planets with minimum masses of 1.02 \ > M _ { Jup } and 4.58 M _ { Jup } , and periods of 415 \ > { d } and 964 \ > { d } , respectively .
The star has the second lowest metallicity among the giant stars hosting more than two planets .
Dynamical stability analysis for the \gamma Lib system sets a minimum orbital inclination angle to be about 70 ^ { \circ } and suggests that the planets are in 7:3 mean-motion resonance , though the current best-fitted orbits to the radial-velocity data are not totally regular .