Hungaria asteroids

[citation needed] Most Hungarias are E-type asteroids, which means they have extremely bright enstatite surfaces and albedos typically above 0.30.

Interior to this 4:1 resonance, asteroids in low inclination orbits are, unlike those outside the 4:1 Kirkwood gap, strongly influenced by the gravitational field of Mars.

[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.

[6] Long-term changes in the orbit of Mars are believed to be a critical factor in the current removal of Hungaria asteroids.

[8] 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.

Asteroid groups out to the orbit of Jupiter, showing eccentricity versus semi-major axis. Hungaria asteroids are the left-most dense grouping in blue. The core region of the asteroid belt is shown in red.
Same as above, but showing inclination versus semi-major axis. Hungaria asteroids are the (top-)left-most dense grouping in blue.
Eccentricity versus semi-major axis: Former location of the hypothetical E-belt asteroids (green outline), with current main belt asteroids (red dots) and Hungaria asteroids (green dots).