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We consider a planetary system consisting of two primaries, namely a star anda giant planet, and a massless secondary, say a terrestrial planet or anasteroid, which moves under their gravitational attraction. We study thedynamics of this system in the framework of the circular and ellipticrestricted TBP, when the motion of the giant planet describes circular andelliptic orbits, respectively. Originating from the circular family, familiesof symmetric periodic orbits in the 3/2, 5/2, 3/1, 4/1 and 5/1 mean-motionresonances are continued in the circular and the elliptic problems. Newbifurcation points from the circular to the elliptic problem are found for eachof the above resonances and thus, new families, continued from these points areherein presented. Stable segments of periodic orbits were found at higheccentricity values of the already known families considered as whole unstablepreviously. Moreover, new isolated (not continued from bifurcation points)families are computed in the elliptic restricted problem. The majority of thenew families mainly consist of stable periodic orbits at high eccentricities.The families of the 5/1 resonance are investigated for the first time in therestricted three-body problems. We highlight the effect of stable periodicorbits on the formation of stable regions in their vicinity and unveil theboundaries of such domains in phase space by computing maps of dynamicalstability. The long-term stable evolution of the terrestrial planets orasteroids is dependent on the existence of regular domains in their dynamicalneighbourhood in phase space, which could host them for long time spans. Thisstudy, besides other celestial architectures that can be efficiently modelledby the circular and elliptic restricted problems, is particularly appropriatefor the discovery of terrestrial companions among the single-giant planetsystems discovered so far.

Origin and continuation of 3/2, 5/2, 3/1, 4/1 and 5/1 resonant periodic orbits in the circular and elliptic restricted three-body problem