Lifetimes of small bodies in planetocentric (or heliocentric) orbits

Dobrovolskis, Anthony R.; Alvarellos, J. L.; Lissauer, Jack J.

doi:10.1016/j.icarus.2006.11.024

Cited by 23 publications

(25 citation statements)

References 34 publications

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“…The power law function is a good fit, but with a small exponent D, which makes it practically similar to a logarithmic decay. The best fit stretched exponential value of β obtained here is much smaller than the value of ∼ 0.3-0.5 obtained by many of the cases shown by Dobrovolskis et al (2007). This may indicate that classical diffusion does not dominate the loss of asteroids from the main belt.…”

Section: Empirical Models Of Population Decaycontrasting

confidence: 71%

Dynamical erosion of the asteroid belt and implications for large impacts in the inner Solar System

Minton

Malhotra

2010

Icarus

162

155

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The cumulative effects of weak resonant and secular perturbations by the major planets produce chaotic behavior of asteroids on long timescales. Dynamical chaos is the dominant loss mechanism for asteroids with diameters Our model suggests that the rate of impacts from large asteroids has declined by a factor of 3 over the last 3 Gy, and that the present-day impact flux of D > 10 km objects on the terrestrial planets is roughly an order of magnitude less than estimates currently in use in crater chronologies and impact hazard risk assessments.

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Section: Empirical Models Of Population Decaycontrasting

confidence: 71%

Dynamical erosion of the asteroid belt and implications for large impacts in the inner Solar System

Minton

Malhotra

2010

Icarus

162

155

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“…We found that the decay profiles of the EV and EM belts can be fit rather well with the Kohlrausch law, whose funtional form is given by (Dobrovolskis et al 2007)…”

Section: Decay Profilesmentioning

confidence: 74%

The terrestrial Planet V hypothesis as the mechanism for the origin of the late heavy bombardment

Brasser

Morbidelli

2011

A&A

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In this study we attempt to model, with numerical simulations, the scenario for the origin of the late heavy bombardment (LHB) proposed in Chambers (2007, Icarus, 189, 386). Chambers suggested that the orbit of a fictitious sub-Mars sized embryo outside Mars became unstable and crossed a part of the asteroid belt until it was removed through ejection or collision. Chambers demonstrated that this kind of evolution can occur at the LHB time, but he did not check whether enough material could be liberated from the belt to be consistent with the magnitude of the LHB. We do that here. In addition to the asteroid belt, we also consider putative belts of small objects located between the orbits of the Earth and Venus (EV belt) or between the Earth and Mars (EM belt). We find that delivering enough material to the Moon from the asteroid belt requires at least a 5 lunar mass embryo crossing the entire asteroid belt up to 3.3 AU for longer than 300 Myr on a low-inclination orbit. We do not witness this to occur in over a hundred simulations. An alternative approach, which relies only on decimating the inner belt (<2.5 AU), requires that the inner belt originally contained 4 to 13 times more mass than the original outer belt. Regarding the putative asteroid belts in between the terrestrial planets, this scenario could be consistent with the LHB if EV belt contained a substantial population of small bodies, with the density of objects in orbital space larger than that of the current main asteroid belt, while the EM belt was as good as empty.

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“…As described in the previous section, the number of planetesimals decreases while the eand i-distributions approach the isotropic distribution. We fit the decay curve empirically using the standard exponential decay curve and the stretched exponential decay defined by the Kohlrausch formula (Dobrovolskis et al 2007).…”

Section: Decay Of Comet Cloudsmentioning

confidence: 99%

Effect of Stellar Encounters on Comet Cloud Formation

Higuchi

Kokubo

2015

The Astronomical Journal

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We have investigated the effect of stellar encounters on the formation and disruption of the Oort cloud using the classical impulse approximation. We calculate the evolution of a planetesimal disk into a spherical Oort cloud due to the perturbation from passing stars for 10 Gyr. We obtain the empirical fits of the e-folding time for the number of Oort cloud comets using the standard exponential and Kohlrausch formulae as functions of the stellar parameters and the initial semimajor axes of planetesimals. The e-folding time and the evolution timescales of the orbital elements are also analytically derived. In some calculations, the effect of the Galactic tide is additionally considered. We also show the radial variations of the e-folding times to the Oort cloud. From these timescales, we show that if the initial planetesimal disk has the semimajor axes distribution dn/da ∝ a −2 , which is produced by planetary scattering (Higuchi et al. 2006), the e-folding time for planetesimals in the Oort cloud is ∼10 Gyr at any heliocentric distance r. This uniform e-folding time over the Oort cloud means that the supply of comets from the inner Oort cloud to the outer Oort cloud is sufficiently effective to keep the comet distribution as dn/dr ∝ r −2 . We also show that the final distribution of the semimajor axes in the Oort cloud is approximately proportional to a −2 for any initial distribution.

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Lifetimes of small bodies in planetocentric (or heliocentric) orbits

Cited by 23 publications

References 34 publications

Dynamical erosion of the asteroid belt and implications for large impacts in the inner Solar System

Dynamical erosion of the asteroid belt and implications for large impacts in the inner Solar System

The terrestrial Planet V hypothesis as the mechanism for the origin of the late heavy bombardment

Effect of Stellar Encounters on Comet Cloud Formation

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