"Hungaria asteroid" redirects here. For the namesake asteroid from which the group takes its name, see 434 Hungaria.
The Hungaria asteroids, also known as the Hungaria group, are 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]
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.
The Hungaria asteroids typically share the following orbital parameters:[1][2]
Approximate mean-motion resonance with Jupiter of 9:2, and with Mars of 2:3
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).[citation needed]
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.[citation needed]
E-beltedit
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).
^ abcSpratt, 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.
^ abWarner, 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.
^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.
^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.
^Milani, Andrea; Knezevic, Zoran; Novakovic, Bojan; Cellino, Alberto (June 2010). (PDF). Icarus. 207 (2): 769–794. Bibcode:2010Icar..207..769M. CiteSeerX10.1.1.151.6659. doi:10.1016/j.icarus.2009.12.022. S2CID 17409201. Archived from the original (PDF) on 2018-02-22. Retrieved 25 August 2018.
^Vitagliano, Aldo (2007). . Archived from the original on 2007-09-07.
^Bottke, Bill (2011-08-14). "Late, Late Heavy Bombardment - Bill Bottke (SETI Talks)". YouTube. SETI Institute.
External linksedit
Hungaria group
Orbital diagram, EasySky
November 26, 2023
hungaria, asteroids, hungaria, asteroid, redirects, here, namesake, asteroid, from, which, group, takes, name, hungaria, also, known, hungaria, group, dynamical, group, asteroids, asteroid, belt, which, orbit, with, semi, major, axis, longest, radius, ellipse,. Hungaria asteroid redirects here For the namesake asteroid from which the group takes its name see 434 Hungaria The Hungaria asteroids also known as the Hungaria group are 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 Contents 1 Description 2 E belt 3 See also 4 References 5 External linksDescription edit nbsp 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 nbsp Same as above but showing inclination versus semi major axis Hungaria asteroids are the top left most 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 2 3The 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 citation needed 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 citation needed E belt edit nbsp 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 These dispersed E belt asteroids might in turn have been the impactors of the Late Heavy Bombardment citation needed See also editE type asteroid Aubrite 434 Hungaria 1025 Riema 1103 Sequoia 1453 Fennia 1750 Eckert 7187 IsobeReferences edit a b c 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 a b Warner Brian D Harris Alan W Vokrouhlicky David Nesvorny 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 Cuk Matija Gladman Brett J Nesvorny 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 Galiazzo Mattia A Bazso Akos 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 amp SS 84 5G doi 10 1016 j pss 2013 03 017 Asteroid lightcurves Archived 2007 10 08 at the Wayback Machine 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 S2CID 17409201 Archived from the original PDF on 2018 02 22 Retrieved 25 August 2018 Vitagliano Aldo 2007 Distance of Mars from Earth Archived from the original on 2007 09 07 Bottke Bill 2011 08 14 Late Late Heavy Bombardment Bill Bottke SETI Talks YouTube SETI Institute External links editHungaria group Orbital diagram EasySky Retrieved from https en wikipedia org w index php title Hungaria asteroids amp oldid 1181770641, wikipedia, wiki, book, books, library,
