Maps of secular resonances in the NEO region

Fenucci, Marco; Gronchi, Giovanni F.; Novaković, Bojan

doi:10.1051/0004-6361/202245546

Cited by 3 publications

(1 citation statement)

References 42 publications

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“…The outer peak is due to a number of resonances with the giant planets (i.e., ν 5 , ν 6 , and the 3:1 meanmotion resonance with Jupiter (Moons & Morbidelli 1995;Michel & Froeschlé 1997;Gladman et al 2000)). The ν 5 resonance is also present at higher inclinations at the peak near 1.5 au (Michel & Froeschlé 1997;Fenucci et al 2023). Since these disks start out with a wide range of inclinations, these resonances still have a significant effect in this area.…”

Section: Evolution Of Simulationsmentioning

confidence: 94%

Forming Mercury from Excited Initial Conditions

Scora,

Valencia,

Morbidelli

et al. 2024

ApJ

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Mercury is notoriously difficult to form in Solar System simulations, due to its small mass and iron-rich composition. Smooth particle hydrodynamics simulations of collisions have found that a Mercury-like body could be formed by one or multiple giant impacts, but due to the chaotic nature of collisions, it is difficult to create a scenario where such impacts will take place. Recent work has found more success forming Mercury analogues by adding additional embryos near Mercury’s orbit. In this work, we aim to form Mercury by simulating the formation of the Solar System in the presence of the giant planets Jupiter and Saturn. We test out the effect of an inner disk of embryos added on to the commonly used narrow annulus of initial material. We form Mercury analogues with core-mass fractions (CMFs) > 0.4 in ∼10% of our simulations, and twice that number of Mercury analogues form during the formation process but are unstable and do not last to the end of the simulations. Mercury analogues form at similar rates for both disks with and without an inner component, and most of our Mercury analogues have lower CMFs than that of Mercury, ∼0.7, due to significant accretion of debris material. We suggest that a more in-depth understanding of the fraction of debris mass that is lost to collisional grinding is necessary to understand Mercury’s formation, or some additional mechanism is required to stop this debris from accreting.

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Section: Evolution Of Simulationsmentioning

confidence: 94%

Forming Mercury from Excited Initial Conditions

Scora,

Valencia,

Morbidelli

et al. 2024

ApJ

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Identifying parent bodies of meteorites among near-Earth asteroids

Carbognani¹,

Fenucci

2023

Monthly Notices of the Royal Astronomical Society

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Meteorites provide an important source of information about the formation and composition of asteroids, because the level of accuracy of studies and analyses performed in a laboratory cannot be achieved by any ground or space based observation. To better understand what asteroid types a meteorite represents, it is crucial to identify the body they originated from. In this paper, we aim to determine possible parent bodies for the known meteorite falls among the known population of near-Earth asteroids (NEAs). By using the similarity criterion DN, based on geocentric quantities, we found 20 possible NEA-meteorite pairs. By performing additional numerical simulations of the backward dynamics, we found that 12 of these pairs may be associated with a possible separation event from the progenitor NEA, while the remaining 8 pairs appear to be ambiguous or random associations. The most interesting are the Pribram and Neuschwanstein meteorites, which are dynamically associated with (482488) 2012 SW20 with a common separation age dating back to about 20−30 kyr ago, and the Motopi Pan meteorite, that has three candidate parent bodies: (454100) 2013 BO73, 2017 MC3, and 2009 FZ4. The average time of separation between our meteorite list and the progenitor body appears to be about 10 kyr, a time consistent with what is expected from the collision frequency of small NEAs. Based on our results, we suggest that about 25 per cent of meteorites do not originate in the main belt, but mainly from little collision events happening between NEAs in the inner Solar System.

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Long-term orbital evolution of dimorphos boulders and implications on the origin of meteorites

Fenucci,

Carbognani

2024

Monthly Notices of the Royal Astronomical Society

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By using recent observations of the Dydimos−Dimorphos system from the Hubble Space Telescope, 37 boulders with a size of 4 to 7 meters ejected from the system during the impact with the DART spacecraft were identified. In this work, we studied the orbital evolution of a swarm of boulders with a similar size to that of the detected ones. By using recent estimates for the ejection velocity of the boulders, we numerically propagated the dynamics of the swarm for 20 kyr in the future. We found that the ejection velocities and the non-gravitational effects are not strong enough to change the secular evolution significantly. The minimum orbit intersection distance (MOID) with the Earth will be reached in about 2.5 kyr, but it will not fall below 0.02 au. On the contrary, the Mars MOID will be very small in four instances, two near 6 kyr and the other two near 15 kyr. Therefore, there may be a chance for them to impact Mars in the future. Given the rarefaction of the Martian atmosphere, we expect the boulders to arrive intact on the ground and excavate a small impact crater. The results presented here provide a further indication that some meteorites found on Earth originated in collisions of ∼100 m near-Earth asteroids with projectiles of ∼1 m in size.

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Maps of secular resonances in the NEO region

Cited by 3 publications

References 42 publications

Forming Mercury from Excited Initial Conditions

Forming Mercury from Excited Initial Conditions

Identifying parent bodies of meteorites among near-Earth asteroids

Long-term orbital evolution of dimorphos boulders and implications on the origin of meteorites

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