orbit of Mars and are still in the process of being ejected from the Solar System due to Mars's influence (unlike asteroids in the "core" of the asteroid belt, where Jupiter's influence predominates). Long-term changes in the orbit of Mars are believed to be a critical factor in the current removal of Hungaria asteroids. At the highest eccentricities, similar to the extreme values observed today or even slightly greater, Mars will perturb Hungaria asteroids and force them into ever more eccentric and unstable orbits when their ascending node is close in longitude to Mars's aphelion. This ultimately leads over millions of years to the formation of the short-lived Amor asteroids and Earth-crossers. E-belt The Hungaria asteroids are thought to be the remains of the hypothetical E-belt asteroid population. The dispersal of most of that hypothetical E-belt might have been caused by the outwards migration of the giant planets of the Solar System, according to simulations done under the Nice model. These dispersed E-belt asteroids might in turn have been the impactors of the Late Heavy Bombardment. See also E-type asteroid Aubrite 434 Hungaria 1025 Riema 1103 Sequoia 1453 Fennia 1750 Eckert 7187 Isobe References External links Hungaria group Orbital diagram, EasySky Asteroid groups and families