The evolution of stars and their hosting binary systems is a highly interactive process and cannot be investigated in a segregated manner. Due to the constraints drawn by stellar binarity, oscillating red-giant stars in binary systems represent a unique opportunity to study the details of the structure and evolution of stars in the advanced phases of stellar evolution. Until recently, the number of known systems hosting solarlike oscillators was small. In this poster, we present the joint analysis of space photometry from NASA Kepler and TESS, ground-based high-resolution spectroscopy such as APOGEE, and astrometry and orbital solutions from space with the ESA Gaia satellite (DR3). Our new approach delivered ~1000 new solar-like oscillators in binary systems with known orbital solutions and increased the sample size by an order of magnitude. From the large sample, we can follow the evolution of the orbital eccentricity of a solar-like star as a function of age. Using asteroseismic techniques, we can distinguish between the various evolutionary phases and identify changes in the period and eccentricity of the orbit and stellar activity due to the accumulated effects of stellar evolution and tidal star-star interaction.