TheHungaria asteroids, also known as theHungaria group, are a dynamical group ofasteroids in theasteroid belt[1] whichorbit the Sun with asemi-major axis (longest radius of an ellipse) between 1.78 and 2.00astronomical units (AU).[2] They are the innermost dense concentration of asteroids in theSolar System—thenear-Earth asteroids are much more sparse—and derive their name from their largest member434 Hungaria. The Hungaria group includes theHungaria family (FIN:003), a collisionalasteroid family which dominates its population.[3][4]
The Hungaria asteroids typically share the followingorbital parameters:[1][2]
The 4:1 resonanceKirkwood gap (at 2.06 AU) marks the outer boundary of the Hungaria family, while interactions with Mars determine the inner boundary. For comparison the majority of asteroids are in core region of the asteroid belt, which lies between the 4:1 gap (at 2.06 AU) and the 2:1 gap (at 3.27 AU).[citation needed]
Most Hungarias areE-type asteroids, which means they have extremely brightenstatite surfaces andalbedos typically above 0.30. Despite their high albedos, none can be seen withbinoculars because they are far too small: the largest (434 Hungaria) is only about 11 km in size. They are, however, the smallest asteroids that can regularly be glimpsed with amateur telescopes.[5]
The origin of the Hungaria group of asteroids is well known. At the 4:1 orbital resonance withJupiter that lies atsemi-major axes of 2.06 AU, any orbiting body is sufficiently strongly perturbed to be forced into an extremely eccentric and unstable orbit, creating the innermostKirkwood gap. Interior to this 4:1 resonance, asteroids in lowinclination orbits are, unlike those outside the 4:1 Kirkwood gap, strongly influenced by the gravitational field ofMars. Here, instead of Jupiter's influence, perturbations by Mars have, over the lifetime of the Solar System, thrown out all asteroids interior to the 4:1 Kirkwood gap except for those far enough from Mars's orbital plane where that planet exerts much smaller forces.[1]
This has left a situation where the only remaining concentration of asteroids inward of the 4:1 resonance lies at high inclination orbits, although they have fairly low eccentricities. However, even at the present time in Solar System history, some Hungaria asteroidscross the 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).[6]
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 ascendingnode is close in longitude to Mars'saphelion.[7] This ultimately leads over millions of years to the formation of the short-livedAmor asteroids andEarth-crossers.[citation needed]
The Hungaria asteroids are thought to be the remains of the hypotheticalE-belt asteroid population.[8] The dispersal of most of that hypothetical E-belt might have been caused by theoutwards migration of thegiant planets of theSolar System, according to simulations done under theNice model. These dispersed E-belt asteroids might in turn have been the impactors of theLate Heavy Bombardment.[citation needed]