Hecuba-gap asteroid

A Hecuba-gap asteroid is a member of a dynamical group of resonant asteroids located in the Hecuba gap at 3.27 AU – one of the largest Kirkwood gaps in the asteroid belt, which is considered the borderline separating the outer main belt asteroids from the Cybeles. A Hecuba-gap asteroid stays in a 2:1 mean motion resonance with the gas giant Jupiter, which may gradually perturbe its orbits over a long period until it either intersect with the orbit of Mars or Jupiter itself. Depending on the dynamical stability of an asteroid's orbit in the Hecuba gap, three subgroups have been proposed. These are the marginally unstable Griqua asteroids, with an estimated lifetime of more than 100 million years, the stable Zhongguo asteroids (more than 500 million or even 1 billion years), and an unnamed, strongly unstable population of asteroids with a dynamical lifetime of less than 70 million years.^[1]^[2]^[3]

Moving further out the Solar System, the asteroids in the Hecuba gap are followed by the resonant Cybeles (7:4), Hildas (3:2), Thules (4:3) and Jupiter trojans (1:1).

Description

Both the Zhongguo (stable) and Griqua asteroids (marginally stable) are also described as the "long-lived" group with lifetimes over 70 million years in order to distinct them from the "short-lived" population. The division between the Griquas and Zhongguo into clearly distinct groups in terms of lifetime has also been questioned and follow-up studies have moved the threshold lifetime between the two long-lived groups from 500 million to 1 billion years.^[2]

Griqua asteroids

The Griqua asteroids (also known as the "Griquas") are a dynamical group of asteroids with marginally unstable orbits. The group derives its name from the asteroid 1362 Griqua. The Griquas are located in the Hecuba gap – one of the largest Kirkwood gaps in the asteroid belt at 3.27 AU – and stay in a 2:1 mean motion resonance with the gas giant Jupiter, which gradually perturbes their orbits over a long period until they either intersect with the orbit of Mars or Jupiter itself. The group has an estimated lifetime of 100 to (at least) 500 million years. Known members of the Griqua group include (articles in boldface):^[1]^: 422

Zhongguo asteroids

While the Griquas are asteroids in a marginally unstable orbit, the Zhongguo asteroids (or "Zhongguos"; named after 3789 Zhongguo) are in a rather stable 1:2 resonance with Jupiter. The group of 26 identified members, with a lifetime of more than 530 million (or even 1 billion^[2]) years, can be further divided into two clusters in the pseudo-proper element space:^[1]^: 423

Strongly unstable group

Related but distinct from the "long-lived" Griquas and Zhongguos, is the group of "unstable" Hecuba-gap asteroids:^[1]^{: 422, 423}

In 2005, further research expanded this group of 16 bodies with an additional 31 multi-opposition asteroids, that show life-times of less than 70 million years. It is also thought that approximately 25% of the short-lived population are "extremely unstable" with lifetimes of less than 2 million years.^[2]

Among the unstable population, some asteroids have such a high eccentricity with a perihelion of less than 1.3 AU, that qualifies them as a near-Earth object. These five bodies (with their current eccentricity taken from the JPL SBDB in parentheses) are 5370 Taranis (0.64), 1995 QN₃ (0.65), 2003 UL₁₂ (0.70), 1997 YM₃ (0.66), 2000 WL₁₀ (0.72).^[2]

References

^ ^a ^b ^c ^d Roig, F.; Nesvorný, D.; Ferraz-Mello, S. (September 2002). "Asteroids in the 2 : 1 resonance with Jupiter: dynamics and size distribution [ Erratum: 2002MNRAS.336.1391R ]". Monthly Notices of the Royal Astronomical Society. 335 (2): 417–431. Bibcode:2002MNRAS.335..417R. doi:10.1046/j.1365-8711.2002.05635.x.
^ ^a ^b ^c ^d ^e Broz, M.; Vokrouhlický, D.; Roig, F.; Nesvorný, D.; Bottke, W. F.; Morbidelli, A. (June 2005). "Yarkovsky origin of the unstable asteroids in the 2/1 mean motion resonance with Jupiter". Monthly Notices of the Royal Astronomical Society. 359 (4): 1437–1455. Bibcode:2005MNRAS.359.1437B. doi:10.1111/j.1365-2966.2005.08995.x.
^ Chrenko, O.; Broz, M.; Nesvorný, D.; Tsiganis, K.; Skoulidou, D. K. (August 2015). "The origin of long-lived asteroids in the 2:1 mean-motion resonance with Jupiter". Monthly Notices of the Royal Astronomical Society. 451 (3): 2399–2416. arXiv:1505.04329. Bibcode:2015MNRAS.451.2399C. doi:10.1093/mnras/stv1109.

External links

On the Origin of the Long-Lived Asteroids in the 2:1 Mean-Motion Resonance with Jupiter, 8-slide presentation, Chrenko, 2014
Dynamics of the Solar System – Publication overview, Miroslav Broz, Institute of Astronomy, Charles University
EasySky, orbital diagram
Minor planet groups/families, www.projectpluto.com

[Roig-2002-1] Roig, F.; Nesvorný, D.; Ferraz-Mello, S. (September 2002). "Asteroids in the 2 : 1 resonance with Jupiter: dynamics and size distribution [ Erratum: 2002MNRAS.336.1391R ]". Monthly Notices of the Royal Astronomical Society. 335 (2): 417–431. Bibcode:2002MNRAS.335..417R. doi:10.1046/j.1365-8711.2002.05635.x.

[Broz-2005-2] Broz, M.; Vokrouhlický, D.; Roig, F.; Nesvorný, D.; Bottke, W. F.; Morbidelli, A. (June 2005). "Yarkovsky origin of the unstable asteroids in the 2/1 mean motion resonance with Jupiter". Monthly Notices of the Royal Astronomical Society. 359 (4): 1437–1455. Bibcode:2005MNRAS.359.1437B. doi:10.1111/j.1365-2966.2005.08995.x.

[Chrenko-2015-3] Chrenko, O.; Broz, M.; Nesvorný, D.; Tsiganis, K.; Skoulidou, D. K. (August 2015). "The origin of long-lived asteroids in the 2:1 mean-motion resonance with Jupiter". Monthly Notices of the Royal Astronomical Society. 451 (3): 2399–2416. arXiv:1505.04329. Bibcode:2015MNRAS.451.2399C. doi:10.1093/mnras/stv1109.

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