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We report the detection of planets around two evolved giant stars from radialvelocity measurements at Okayama Astrophysical observatory. 24 Boo (G3IV) has amass of $0.99\,M_{\odot}$, a radius of $10.64\,R_{\odot}$, and a metallicity of${\rm [Fe/H]}=-0.77$. The star hosts one planet with a minimum mass of$0.91\,M_{\rm Jup}$ and an orbital period of $30.35{\rm d}$. The planet has oneof the shortest orbital periods among those ever found around evolved stars byradial-veloocity methods. The stellar radial velocities show additionalperiodicity with $150{\rm d}$, which are probably attributed to stellaractivity. The star is one of the lowest-metallicity stars orbited by planetscurrently known. $\gamma$ Lib (K0III) is also a metal-poor giant with a mass of$1.47\,M_{\odot}$, a radius of $11.1\,R_{\odot}$, and ${\rm [Fe/H]}=-0.30$. Thestar hosts two planets with minimum masses of $1.02M_{\rm Jup}$ and$4.58\,M_{\rm Jup}$, and periods of $415{\rm d}$ and $964{\rm d}$,respectively. The star has the second lowest metallicity among the giant starshosting 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 thecurrent best-fitted orbits to the radial-velocity data are not totally regular.

Planets around the evolved stars 24 Booties and $\gamma$ Libra: A 30d-period planet and a double giant-planet system in possible 7:3 MMR