Updated collisional probabilities of minor body populations

Dell’Oro, A.; Marzari, F.; Paolicchi, Paolo; Vanzani, V.

doi:10.1051/0004-6361:20000492

Cited by 51 publications

(47 citation statements)

References 14 publications

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“…The values obtained for (136108) 2003 EL 61 are P i = 1.47 ± 0.02 × 10 −22 km −2 yr −1 and V col = 2.48 ± 0.86 km s −1 . These values are different from the mean collisional velocity and mean intrinsic collisional probability found by Dell'Oro et al (2001) for the TNOs, but it is a consequence of the excited orbit of this object in comparison with the mean orbit of this population. The projectile collision velocities for the simulation were taken from the collision velocity distribution found for this object, which is shown in Fig.…”

Section: The Modelcontrasting

confidence: 87%

The trans-Neptunian object size distribution at small sizes

Gil-Hutton¹,

Licandro

Pinilla-Alonso

et al. 2009

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Aims. The aim of this work is to estimate the size distribution of small Trans-Neptunian objects. Methods. We simulate the irradiation and collisional processes affecting the surface of a Trans-Neptunian object for the first time using as a constraint the peculiar crystalline to amorphous water ice ratio observed on (136108) 2003 EL 61 . Results. We find that the size distribution changes its exponent from q 0 = 4.2 at larger sizes to q 1 = 2.40 ± 0.3 at the smaller ones, with a break radius of r 1 = 35 ± 15 km. If this size distribution is applied to studying the collisional surface evolution of (136108) 2003 EL 61 , we find that the object must be covered by a thin ice crust of ≈0.12 cm, while the original composition of the object is still present at 1.61 cm or more below the surface. This result is not affected by a collision with a large projectile that occurred by chance more than 10 9 yr ago since after a short time the mean value obtained for the crystalline to amorphous water ice ratio is indistinguishable from the one obtained without a collision with a large projectile. Since the simulations are not sensitive to the effects of very small projectiles (r p < 10−30 m), it is possible that the exponent of the size distribution for these very small objects changes again, approaching a Donhanyi's size distribution.

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Section: The Modelcontrasting

confidence: 87%

The trans-Neptunian object size distribution at small sizes

Gil-Hutton¹,

Licandro

Pinilla-Alonso

et al. 2009

A&A

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“…A previous computation of the probability of collisions among TNOs has been done by Dell'Oro et al (2001). At that time the number of known TNOs was much smaller than nowadays and no model nor extrapolation for the entire population was available.…”

Section: Discussionmentioning

confidence: 99%

“…The approach has been successfully used for the computation of the probabilities of impact among some orbits in resonant conditions like the case Jupiter Trojans (Dell'Oro & Paolicchi 1998b) and the case of Plutinos (Dell'Oro et al 2001). In the simple case of collisions between two bodies, the computation of the intrinsic probability of collision is based on the numerical evaluation of a surface integral in the space of the six angular orbital elements of the target f t , ω t , Ω t and the projectile f p , ω p , Ω p , where f is true anomaly (see Dell'Oro & Paolicchi 1998a, for details).…”

Section: The Computational Toolmentioning

confidence: 99%

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Statistics of encounters in the trans-Neptunian region

Dell’Oro

Bagatín

Benavídez

et al. 2013

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The inventory of the populations of trans-Neptunian objects (TNO) has grown considerably over the last decade. As for other groups of small bodies in our solar system, TNOs are expected to have experienced a collisional evolution owing to their mutual impacts. The knowledge of the statistics of collisions, including determination of the rate of mutual collisions and the distribution of the impact velocity, is indeed a fundamental prerequisite for developing models of collisional evolution. We revised the evaluation of those statistical parameters for TNOs provided more than ten years ago on the basis of a much more limited sample of objects than currently available. We used the Canada-France Ecliptic Plane Survey (CFEPS) L7 model to extract an unbiased sample of orbits for TNOs, while the statistical parameters of impact are computed using a statistical tool. We investigated the statistics of impacts among TNOs for the whole population and for different dynamical subgroups. Moreover, we investigated the statistics of collisions between subgroups with crossing orbits. The peculiar dynamical behavior of objects in resonant orbits is taken into account. Our present computation of the probabilities of collision are 20% to 50% lower than previous estimates, while mean impact velocities turn out to be about 70% higher. For instance, the rate of collisions among Plutinos, expressed in terms of the so-called mean intrinsic probability of collision, results to be (3.90 ± 0.01) × 10 −22 km −2 yr −1 and the mean impact velocity is 2.46 ± 0.01 km s −1 . We also find that the distributions of impact velocities seem to be quite different from pure Maxwellian distributions. These results can be useful in developing models of the collisional evolution in the trans-Neptunian region.

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“…Finally, we briefly discussed the L 5 jovian Trojan dust. The intrinsic collision probabilities and the mean impact velocities in the L 4 and L 5 swarms have similar values (Dell'Oro et al 1998), so that the collisional evolution of the populations in both swarms should not be very different. Since the number ratio of L 4 to L 5 is 1.3-2.5 (for D > 2 km) (Yoshida & Nakamura 2008), we think that the L 4 dust production should be somewhat greater than the L 5 one.…”

Section: Resultsmentioning

confidence: 96%

Studying the jovian Trojan dust

Elía

Brunini

2010

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Aims. We analyze the jovian Trojan dust in the L 4 swarm. Methods. To do this, we use a modification of the numerical code developed by us and previously applied to the collisional and dynamical evolution of the L 4 jovian Trojans. This algorithm considers catastrophic collisions and cratering events, includes a dynamical treatment that takes the stability and instability zones of the L 4 jovian swarm into account, and incorporates the effects of the Poynting-Robertson radiation.Results. From this analysis, we infer that the time evolution of the L 4 jovian Trojan dust luminosity has the characteristics of a diffusion process, since its current value is fairly insensitive to variations in the initial size distribution. Moreover, our results indicate that the current luminosity of the dust in the L 4 jovian swarm ranges from ∼3.2 × 10 −8 to 3.4 × 10 −8 L . Conclusions. From these estimates, we conclude that the current luminosity of the dust in the L 4 jovian swarm is comparable to the luminosity of the inner Solar System dust, and, at least, one order of magnitude lower than the luminosity of the outer Solar System dust.

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Updated collisional probabilities of minor body populations

Cited by 51 publications

References 14 publications

The trans-Neptunian object size distribution at small sizes

The trans-Neptunian object size distribution at small sizes

Statistics of encounters in the trans-Neptunian region

Studying the jovian Trojan dust

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