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

Delisle, J.-B.; Laskar, Jacques

doi:10.1051/0004-6361/201118339

Cited by 21 publications

(39 citation statements)

References 22 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Orbital diffusion caused by close encounters between small asteroids and one of the major bodies in the main belt, (1) Ceres 1 , (2) Pallas, (4) Vesta, and (10) Hygiea was already shown to be a mechanism able to produce long-term change in the proper elements of asteroids in the proximity of the orbits of (1) Ceres and (4) Vesta (Carruba et al 2003(Carruba et al , 2007Delisle & Laskar 2012). The change in semi-major axis, eccentricity, and inclination caused by the long-term effect of close encounters with (4) Vesta may have contributed to the diffusion of some of the V-type asteroids currently outside the Vesta family whose orbits could not be easily explained in terms of migration from the Vesta family caused by other mechanisms, such as diffusion by the Yarkovsky and YORP effects, interaction with mean-motion and secular resonances, or both.…”

Section: Introductionmentioning

confidence: 99%

“…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. Delisle & Laskar (2012) estimated that close encounters dominated the orbital mobility of minor bodies with respect to the Yarkovsky and YORP effects only for large objects, with increasingly limited diameters when longer timescales were considered.…”

Section: Introductionmentioning

confidence: 99%

“…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. Delisle & Laskar (2012) estimated that close encounters dominated the orbital mobility of minor bodies with respect to the Yarkovsky and YORP effects only for large objects, with increasingly limited diameters when longer timescales were considered. One question left unanswered by the Delisle & Laskar (2012) paper was on the indirect effect of close encounter with massive asteroids when more than one object was considered.…”

Section: Introductionmentioning

confidence: 99%

“…Delisle & Laskar (2012) estimated that close encounters dominated the orbital mobility of minor bodies with respect to the Yarkovsky and YORP effects only for large objects, with increasingly limited diameters when longer timescales were considered. One question left unanswered by the Delisle & Laskar (2012) paper was on the indirect effect of close encounter with massive asteroids when more than one object was considered. It is well known 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.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Chaotic diffusion caused by close encounters with several massive asteroids

Carruba

Huaman

Douwens

et al. 2012

A&A

View full text Add to dashboard Cite

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.

show abstract

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Chaotic diffusion caused by close encounters with several massive asteroids

Carruba

Huaman

Douwens

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…timescales of 250 Myr, according to Delisle & Laskar (2011; see also a discussion in Carruba et al 2003). Using the relationship…”

Section: Dynamical Mapsmentioning

confidence: 99%

Chaotic diffusion caused by close encounters with several massive asteroids

Carruba

Huaman

Domingos

et al. 2013

A&A

View full text Add to dashboard Cite

Context. Close encounters with (1) Ceres and (4) Vesta, the two most massive bodies in the main belt, are known to be a mechanism of dynamical mobility able to 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). Recently, it has been shown that drift rates caused by close encounters with massive asteroids may change significantly on timescales of 30 Myr when different models (i.e., different numbers of massive asteroids) are considered. Aims. So far, not much attention has been given to the case of diffusion caused by the other most massive bodies in the main belt: (2) Pallas, (10) Hygiea, and (31) Euphrosyne, the third, fourth, and one of the most massive highly inclined asteroids in the main belt, respectively. Since (2) Pallas is a highly inclined object, relative velocities at encounter with other asteroids tend to be high and changes in proper elements are therefore relatively small. It was thus believed that the scattering effect caused by highly inclined objects in general should be small. Can diffusion by close encounters with these asteroids be a significant mechanism of long-term dynamical mobility? Methods. By performing simulations with symplectic integrators, we studied the problem of scattering caused by close encounters with (2) Pallas, (10) Hygiea, and (31) Euphrosyne when only the massive asteroids (and the eight planets) are considered, and the other massive main belt asteroids and non-gravitational forces are also accounted for. Results. By finding relatively small values of drift rates for (2) Pallas, we confirm that orbital scattering by this highly inclined object is indeed a minor effect. Unexpectedly, however, we obtained values of drift rates for changes in proper semi-major axis a caused by (10) Hygiea and (31) Euphrosyne larger than what was previously found for scattering by (4) Vesta. These high rates may have repercussions on the orbital evolution and age estimate of their respective families.

show abstract

V‐type near‐Earth asteroids: Dynamics, close encounters and impacts with terrestrial planets

2017

View full text Add to dashboard Cite

Asteroids colliding with planets vary in composition and taxonomical type. Among Near-Earth Asteroids (NEAs) are the V-types, basaltic asteroids that are classified via spectroscopic observations. In this work, we study the probability of Vtype NEAs colliding with Earth, Mars and Venus, as well as the Moon. We perform a correlational analysis of possible craters produced by V-type NEAs. To achieve this, we performed numerical simulations and statistical analysis of close encounters and impacts between V-type NEAs and the terrestrial planets over the next 10 Myr. We find that V-type NEAs can indeed have impacts with all the planets, the Earth in particular, at an average rate of once per ∼ 12 Myr. There are four candidate craters on Earth that were likely caused by V-type NEAs.

show abstract

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

Cited by 21 publications

References 22 publications

Chaotic diffusion caused by close encounters with several massive asteroids

Chaotic diffusion caused by close encounters with several massive asteroids

Chaotic diffusion caused by close encounters with several massive asteroids

V‐type near‐Earth asteroids: Dynamics, close encounters and impacts with terrestrial planets

Contact Info

Product

Resources

About