Strong chaos induced by close encounters with Ceres and Vesta

Laskar, Jacques; Gastineau, Mickaël; Delisle, J.-B.; Farrés, Ariadna; Fienga, A.

doi:10.1051/0004-6361/201117504

Cited by 153 publications

(211 citation statements)

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“…(10) gives a jump size of 1.3 AU. The probability of such an encounter can be evaluated using the same approach as in Laskar et al (2011). We obtain a number of encounters closer than the diameter of Vesta (without colliding, i.e., farther away than the radius of Vesta) of about 7 × 10 −4 per Gyr and per fragment.…”

Section: Very Close Encountersmentioning

confidence: 99%

“…In the second simulation (S E) the 11 asteroids were considered as the planets and accordingly interact with members of the synthetic Vesta family. Both solutions are integrated over 30 Myr using the symplectic integrator described in Laskar et al (2011) and references therein. The effects of all planets and Pluto are taken into account, as is general relativity.…”

Section: Introductionmentioning

confidence: 99%

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Chaotic diffusion of the Vesta family induced by close encounters with massive asteroids

Delisle

Laskar

2012

A&A

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We numerically estimate the semi-major axis chaotic diffusion of the Vesta family asteroids induced by close encounters with 11 massive main-belt asteroids: (1) Ceres, (2) Pallas, (3) Juno, (4) Vesta, (7) Iris, (10) Hygiea, (15) Eunomia, (19) Fortuna, (324) Bamberga, (532) Herculina, (704) Interamnia. We find that most of the diffusion is caused by Ceres and Vesta. By extrapolating our results, we are able to constrain the global effect of close encounters with all main-belt asteroids. A comparison of this drift estimate with the one expected for the Yarkovsky effect shows that for asteroids whose diameter is larger than about 40 km, close encounters dominate the Yarkovsky effect. Overall, our findings confirm the standard scenario for the history of the Vesta family.

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Section: Very Close Encountersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Chaotic diffusion of the Vesta family induced by close encounters with massive asteroids

Delisle

Laskar

2012

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“…regions characterized by high collision probabilities with one of the most massive asteroids. Recently, Laskar et al (2011) showed that when the five major bodies were included in simulations with all the planets, surprisingly, not only the orbits of the major asteroids were more chaotic, but even the precision with which the orbital elements of the Earth are known was limited to 50 Myr. Delisle & Laskar (2012) investigated the orbital mobility in the Vesta family region caused by close encounters with eleven major asteroids, and found that most of the mobility is caused by encounters with (4) Vesta and (1) Ceres, and is on the order of magnitude of what is found in previous works (Carruba et al 2003(Carruba et al , 2007.…”

Section: Introductionmentioning

confidence: 99%

Chaotic diffusion caused by close encounters with several massive asteroids

Carruba

Huaman

Douwens

et al. 2012

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Context. Close encounters with massive asteroids are known to be a mechanism of dynamical mobility that can significantly alter proper elements of minor bodies, and they are the main source of dynamical mobility for medium-sized and large asteroids (D > 20 km, approximately). Aims. Orbital mobility caused by close encounters with (4) Vesta has been studied in the past and could be a viable mechanism to produce the current orbital location of some of the V-type asteroids currently outside the Vesta family. It is well known, however, that the proper frequencies of precession of pericenter g and longitude of the node s of terrestrial planets change when one or more of the other planets is not considered in the integration scheme. For instance, the g 4 and s 4 frequencies are different when the full solar system is considered or when only Mars and the Jovian planets are accounted for. In this work we consider the effect that including one or more (up to 51) massive asteroids in the integration scheme has on the Vesta orbit, and, indirectly on the statistics of changes in semi-major axis caused by close encounters with this massive asteroid. Methods. By using chaos indicators such as the maximum Lyapunov exponent, and integrations with symplectic integrators able to account for the interaction between a massive asteroid and a mass-less particle, we studied the problem of scattering caused by close encounters with (4) Vesta, when only (4) Vesta (and the eight planets) are considered, and when (4) Vesta and other massive main belt asteroids are also accounted for. Results. We find that (4) Vesta proper frequencies are dependent on the number of other massive asteroids considered in the integration scheme and that, as a result, the whole statistics of encounters with (4) Vesta is also affected. Variances of the change in proper a caused by the four most massive asteroids varied up to 36.3% in the five integration schemes that we used, and the number of encounters that caused the strongest changes in semi-major axis varied up to a factor 2. The indirect effect caused by the presence of other massive asteroids therefore introduces an additional source of uncertainty in estimating the long-term effect of close encounters with massive asteroids that was not accounted for in previous works on the subject, and that strongly affects estimates of its Hurst exponent.

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“…Thus, the Oligo-Miocene presents an opportunity to study the dynamics of a unipolar (Antarctic) icehouse climate state without the overprint of Northern Hemisphere ice sheets on benthic foraminiferal δ 18 O records. Published proxy records of atmospheric CO 2 concentration show a decline from the Oligocene to the Miocene (6, 7) that is broadly contemporaneous with a strong minimum in the ∼2.4-My eccentricity cycle ∼24 My ago (8), which would promote continental ice sheet expansion if radiative forcing was the dominant control on ice volume. Previous studies using drill core records from the deep ocean demonstrate a climatic response to astronomical forcing for the Oligocene (9,10) and parts of the Miocene (11)(12)(13).…”

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confidence: 99%

Evolution of the early Antarctic ice ages

Liebrand

Bakker

Beddow

et al. 2017

Proc. Natl. Acad. Sci. U.S.A.

104

180

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Understanding the stability of the early Antarctic ice cap in the geological past is of societal interest because present-day atmospheric CO2 concentrations have reached values comparable to those estimated for the Oligocene and the Early Miocene epochs. Here we analyze a new high-resolution deep-sea oxygen isotope (δ18O) record from the South Atlantic Ocean spanning an interval between 30.1 My and 17.1 My ago. The record displays major oscillations in deep-sea temperature and Antarctic ice volume in response to the ∼110-ky eccentricity modulation of precession. Conservative minimum ice volume estimates show that waxing and waning of at least ∼85 to 110% of the volume of the present East Antarctic Ice Sheet is required to explain many of the ∼110-ky cycles. Antarctic ice sheets were typically largest during repeated glacial cycles of the mid-Oligocene (∼28.0 My to ∼26.3 My ago) and across the Oligocene−Miocene Transition (∼23.0 My ago). However, the high-amplitude glacial−interglacial cycles of the mid-Oligocene are highly symmetrical, indicating a more direct response to eccentricity modulation of precession than their Early Miocene counterparts, which are distinctly asymmetrical—indicative of prolonged ice buildup and delayed, but rapid, glacial terminations. We hypothesize that the long-term transition to a warmer climate state with sawtooth-shaped glacial cycles in the Early Miocene was brought about by subsidence and glacial erosion in West Antarctica during the Late Oligocene and/or a change in the variability of atmospheric CO2 levels on astronomical time scales that is not yet captured in existing proxy reconstructions.

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Strong chaos induced by close encounters with Ceres and Vesta

Cited by 153 publications

References 19 publications

Chaotic diffusion of the Vesta family induced by close encounters with massive asteroids

Chaotic diffusion of the Vesta family induced by close encounters with massive asteroids

Chaotic diffusion caused by close encounters with several massive asteroids

Evolution of the early Antarctic ice ages

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