The trans-Neptunian object size distribution at small sizes

Gil-Hutton, R.; Licandro, J.; Pinilla-Alonso, N.; Brunetto, R.

doi:10.1051/0004-6361/200811301

Cited by 17 publications

(12 citation statements)

References 57 publications

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“…Thus, our models in this paper match the slope below the break but not the location of the break. Kenyon & Bromley (2004c) demonstrate that stirring from the largest nearby planet sets the 'break radius' (see also Gil-Hutton et al 2009;Fraser 2009). For TNOs, continued stirring by Neptune at 30 AU yields a break at 10-30 km, close to the lower limit inferred from current observations.…”

Section: Discussionmentioning

confidence: 99%

Coagulation Calculations of Icy Planet Formation at 15-150 Au: A Correlation Between the Maximum Radius and the Slope of the Size Distribution for Trans-Neptunian Objects

Kenyon

Bromley

2012

The Astronomical Journal

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We investigate whether coagulation models of planet formation can explain the observed size distributions of transneptunian objects (TNOs). Analyzing published and new calculations, we demonstrate robust relations between the size of the largest object and the slope of the size distribution for sizes 0.1 km and larger. These relations yield clear, testable predictions for TNOs and other icy objects throughout the solar system. Applying our results to existing observations, we show that a broad range of initial disk masses, planetesimal sizes, and fragmentation parameters can explain the data. Adding dynamical constraints on the initial semimajor axis of 'hot' KBOs along with probable TNO formation times of 10-700 Myr restricts the viable models to those with a massive disk composed of relatively small (1-10 km) planetesimals.

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Section: Discussionmentioning

confidence: 99%

Coagulation Calculations of Icy Planet Formation at 15-150 Au: A Correlation Between the Maximum Radius and the Slope of the Size Distribution for Trans-Neptunian Objects

Kenyon

Bromley

2012

The Astronomical Journal

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“…Di Sisto and Brunini (2011) analyzed the number and size-frequency distribution (SFD) of SDOs based on the works of Parker and Kavelaars (2010b,a). They adopted a broken power-law size distribution with a differential index of large objects given by s 1 = 4.7 (Elliot et al 2005), a break at diameters d ∼ 60 km and two limit values for the differential index s 2 = 2.5 and 3.5 for d < 60 km given the uncertainty of the SFD for small objects (Bernstein et al 2004;Gil-Hutton et al 2009;Fraser and Kavelaars 2009;Fuentes and Holman 2008;Fuentes et al 2009). However, the recent discoveries by OSSOS increased the number of small SDOs and Centaurs and allowed for new estimations of the SFD and number of objects.…”

Section: Resultsmentioning

confidence: 99%

Centaur and giant planet crossing populations: origin and distribution

Sisto

Rossignoli

2020

Celest Mech Dyn Astr

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The current giant planet region is a transitional zone where transneptunian objects (TNOs) cross in their way to becoming Jupiter Family Comets (JFCs). Their dynamical behavior is conditioned by the intrinsic dynamical features of TNOs and also by the encounters with the giant planets. We address the Giant Planet Crossing (GPC) population (those objects with 5.2 au < q < 30 au) studying their number and their evolution from their sources, considering the current configuration of the Solar System. This subject is reviewed from previous investigations and also addressed by new numerical simulations of the dynamical evolution of Scattered Disk Objects (SDOs). We obtain a model of the intrinsic orbital element distribution of GPCs. The Scattered Disk represents the main source of prograde GPCs and Centaurs, while the contribution from Plutinos lies between one and two orders of magnitude below that from the SD. We obtain the number and size distribution of GPCs from our model, computing 9600 GPCs from the SD with D > 100 km and ∼ 10 8 with D > 1 km in the current population. The contribution from other sources is considered negligible. The mean lifetime in the Centaur zone is 7.2 Myr, while the mean lifetime of SDOs in the GPC zone is of 68 Myr. The latter is dependent on the initial inclination, being the ones with high inclinations the ones that survive the longest in the GPC zone. There is also a correlation of lifetime with perihelion distance, where greater perihelion leads to longer lifetime. The dynamical evolution of observed GPCs is different for prograde and retrograde objects. Retrograde GPCs have lower median lifetime than prograde ones, thus experiencing a comparatively faster evolution. However, it is probable that this faster evolution is due to the fact that the majority of retrograde GPCs have low perihelion values and then, lower lifetimes.

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“…An alternative scenario might be the collisional resurfacing, which may explain other phenomena in the transneptunian belt (Gil-Hutton 2002;Gil-Hutton et al 2009). …”

Section: Discussionmentioning

confidence: 99%

Transneptunian objects and Centaurs from light curves

Duffárd¹,

Ortiz²,

Thirouin³

et al. 2009

A&A

101

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Aims. We compile and analyze an extended database of light curve parameters scattered in the literature to search for correlations and study physical properties, including internal structure constraints. Methods. We analyze a vast light curve database by obtaining mean rotational properties of the entire sample, determining the spin frequency distribution and comparing those data with a simple model based on hydrostatic equilibrium. Results. For the rotation periods, the mean value obtained is 6.95 h for the whole sample, 6.88 h for the Trans-neptunian objects (TNOs) alone and 6.75 h for the Centaurs. From Maxwellian fits to the rotational frequencies distribution the mean rotation rates are 7.35 h for the entire sample, 7.71 h for the TNOs alone and 8.95 h for the Centaurs. These results are obtained by taking into account the criteria of considering a single-peak light curve for objects with amplitudes lower than 0.15 mag and a double-peak light curve for objects with variability >0.15 mag. We investigate the effect of using different values other than 0.15 mag for the transition threshold from albedo-caused light curves to shape-caused light curves. The best Maxwellian fits were obtained with the threshold between 0.10 and 0.15 mag. The mean light-curve amplitude for the entire sample is 0.26 mag, 0.25 mag for TNOs only, and 0.26 mag for the Centaurs. The Period versus B − V color shows a correlation that suggests that objects with shorter rotation periods may have suffered more collisions than objects with larger ones. The amplitude versus H v correlation clearly indicates that the smaller (and collisionally evolved) objects are more elongated than the bigger ones.Conclusions. From the model results, it appears that hydrostatic equilibrium can explain the statistical results of almost the entire sample, which means hydrostatic equilibrium is probably reached by almost all TNOs in the H range [−1,7]. This implies that for plausible albedos of 0.04 to 0.20, objects with diameters from 300 km to even 100 km would likely be in equilibrium. Thus, the great majority of objects would qualify as being dwarf planets because they would meet the hydrostatic equilibrium condition. The best model density corresponds to 1100 kg/m 3 .

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The trans-Neptunian object size distribution at small sizes

Cited by 17 publications

References 57 publications

Coagulation Calculations of Icy Planet Formation at 15-150 Au: A Correlation Between the Maximum Radius and the Slope of the Size Distribution for Trans-Neptunian Objects

Coagulation Calculations of Icy Planet Formation at 15-150 Au: A Correlation Between the Maximum Radius and the Slope of the Size Distribution for Trans-Neptunian Objects

Centaur and giant planet crossing populations: origin and distribution

Transneptunian objects and Centaurs from light curves

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