Hungaria asteroids

The Hungaria asteroids, also known as the Hungaria group, is a dynamical group of asteroids in the asteroid belt[1] which orbit the Sun with a semi-major axis (longest radius of an ellipse) between 1.78 and 2.00 astronomical units (AU).[2] They are the innermost dense concentration of asteroids in the Solar System—the near-Earth asteroids are much more sparse—and derive their name from their largest member 434 Hungaria. The Hungaria group includes the Hungaria family (FIN: 003), a collisional asteroid family which dominates its population.[3][4]

"Hungaria asteroid" redirects here. For the namesake asteroid from which the group takes its name, see 434 Hungaria.

Description
Asteroid groups out to the orbit of Jupiter, showing eccentricity versus semi-major axis. Hungaria asteroids are the leftmost dense grouping in blue. The core region of the asteroid belt is shown in red.
Same as above, however showing inclination versus semi-major axis. Again Hungaria asteroids are the (top-)leftmost dense grouping in blue.

The Hungaria asteroids typically share the following orbital parameters:[1][2]

  • Semi-major axis between 1.78 and 2.00 AU
  • Orbital period of approximately 2.5 years
  • Low eccentricity of below 0.18
  • An inclination of 16° to 34°
  • Approximate mean-motion resonance with Jupiter of 9:2, and with Mars of 3:2

The 4:1 resonance Kirkwood 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).

Most Hungarias are E-type asteroids, which means they have extremely bright enstatite surfaces and albedos typically above 0.30. Despite their high albedos, none can be seen with binoculars 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 with Jupiter that lies at semi-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 innermost Kirkwood gap. 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. 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 asteroids cross 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 ascending node is close in longitude to Mars's aphelion.[7] This ultimately leads over millions of years to the formation of the short-lived Amor asteroids and Earth-crossers.

E-belt
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).
Main article: E-belt asteroids

The Hungaria asteroids are thought to be the remains of the hypothetical E-belt asteroid population.[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—and these dispersed E-belt asteroids might in turn have been the impactors of the Late Heavy Bombardment.

See also

References
  1. Spratt, Christopher E. (April 1990). "The Hungaria group of minor planets". Journal of the Royal Astronomical Society of Canada. 84: 123–131. Bibcode:1990JRASC..84..123S. ISSN 0035-872X. Retrieved 25 August 2018.
  2. Warner, Brian D.; Harris, Alan W.; Vokrouhlický, David; Nesvorný, David; Bottke, William F. (November 2009). "Analysis of the Hungaria asteroid population" (PDF). Icarus. 204 (1): 172–182. Bibcode:2009Icar..204..172W. doi:10.1016/j.icarus.2009.06.004. Retrieved 25 August 2018.
  3. Ćuk, Matija; Gladman, Brett J.; Nesvorný, David (2014). "Hungaria asteroid family as the source of aubrite meteorites". Icarus. 239: 154–159. arXiv:1406.0825. Bibcode:2014Icar..239..154C. doi:10.1016/j.icarus.2014.05.048.
  4. Galiazzo, Mattia A.; Bazsó, Ákos; Dvorak, Rudolf (2013). "Fugitives from the Hungaria region: Close encounters and impacts with terrestrial planets". Planetary and Space Science. 84: 5–13. arXiv:1210.1418. Bibcode:2013P&SS...84....5G. doi:10.1016/j.pss.2013.03.017.
  5. Asteroid lightcurves Archived 2007-10-08 at the Wayback Machine
  6. Milani, Andrea; Knezevic, Zoran; Novakovic, Bojan; Cellino, Alberto (June 2010). "Dynamics of the Hungaria asteroids" (PDF). Icarus. 207 (2): 769–794. Bibcode:2010Icar..207..769M. CiteSeerX 10.1.1.151.6659. doi:10.1016/j.icarus.2009.12.022. Retrieved 25 August 2018.
  7. Distance of Mars from Earth Archived 2007-09-07 at the Wayback Machine
  8. Late, Late Heavy Bombardment - Bill Bottke (SETI Talks) – Youtube.com
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