The kilometer-sized Main Belt asteroid population revealed by<i>Spitzer</i>

Ryan, Erin L.; Mizuno, D. R.; Shenoy, S.; Woodward, C. E.; Carey, Sean; Noriega-Crespo, A.; Kraemer, K. E.; Price, S. D.

doi:10.1051/0004-6361/201321375

Cited by 40 publications

(29 citation statements)

References 58 publications

(101 reference statements)

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“…This may steepen to 2.11 ≤ α c ≤ 2.26 when allowing for a distribution of collision velocities (Pan & Schlichting 2012). These values can be compared to the empirical α c of small main belt asteroids, considered to be near steady state (Bottke et al 2005): α c = 3.00 ± 0.05 for 5 < ∼ D < ∼ 40 km (Ivezić et al 2001), α c = 2.55 for 4 < ∼ D < ∼ 27 km if assuming p V = 0.1 (Gladman et al 2009), and α c = 2.34 ± 0.05 for 2 < ∼ D < ∼ 25 km (Ryan et al 2015).…”

Section: Collisional Processingmentioning

confidence: 98%

The primordial nucleus of comet 67P/Churyumov-Gerasimenko

Davidsson

Sierks

Güttler

et al. 2016

A&A

187

169

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Context. We investigate the formation and evolution of comet nuclei and other trans-Neptunian objects (TNOs) in the solar nebula and primordial disk prior to the giant planet orbit instability foreseen by the Nice model. Aims. Our goal is to determine whether most observed comet nuclei are primordial rubble-pile survivors that formed in the solar nebula and young primordial disk or collisional rubble piles formed later in the aftermath of catastrophic disruptions of larger parent bodies. We also propose a concurrent comet and TNO formation scenario that is consistent with observations. Methods. We used observations of comet 67P/Churyumov-Gerasimenko by the ESA Rosetta spacecraft, particularly by the OSIRIS camera system, combined with data from the NASA Stardust sample-return mission to comet 81P/Wild 2 and from meteoritics; we also used existing observations from ground or from spacecraft of irregular satellites of the giant planets, Centaurs, and TNOs. We performed modeling of thermophysics, hydrostatics, orbit evolution, and collision physics. Results. We find that thermal processing due to short-lived radionuclides, combined with collisional processing during accretion in the primordial disk, creates a population of medium-sized bodies that are comparably dense, compacted, strong, heavily depleted in supervolatiles like CO and CO 2 ; they contain little to no amorphous water ice, and have experienced extensive metasomatism and aqueous alteration due to liquid water. Irregular satellites Phoebe and Himalia are potential representatives of this population. Collisional rubble piles inherit these properties from their parents. Contrarily, comet nuclei have low density, high porosity, weak strength, are rich in supervolatiles, may contain amorphous water ice, and do not display convincing evidence of in situ metasomatism or aqueous alteration. We outline a comet formation scenario that starts in the solar nebula and ends in the primordial disk, that reproduces these observed properties, and additionally explains the presence of extensive layering on 67P/Churyumov-Gerasimenko (and on 9P/Tempel 1 observed by Deep Impact), its bi-lobed shape, the extremely slow growth of comet nuclei as evidenced by recent radiometric dating, and the low collision probability that allows primordial nuclei to survive the age of the solar system. Conclusions. We conclude that observed comet nuclei are primordial rubble piles, and not collisional rubble piles. We argue that TNOs formed as a result of streaming instabilities at sizes below ∼400 km and that ∼350 of these grew slowly in a low-mass primordial disk to the size of Triton, Pluto, and Eris, causing little viscous stirring during growth. We thus propose a dynamically cold primordial disk, which prevented mediumsized TNOs from breaking into collisional rubble piles and allowed the survival of primordial rubble-pile comets. We argue that comets formed by hierarchical agglomeration out of material that remained after TNO formation, and that this slow growth was a necessity...

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Section: Collisional Processingmentioning

confidence: 98%

The primordial nucleus of comet 67P/Churyumov-Gerasimenko

Davidsson

Sierks

Güttler

et al. 2016

A&A

187

169

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“…(1) Masiero et al (); (2) Ryan et al (); (3) Yoshida et al (); (4) Delbó et al (); (5) Warner (); (6) Binzel et al (); (7) Mainzer et al (); (8) Taylor et al (); (9) Warner (); (10) Hicks et al (); (11) Somers et al ().…”

Section: Resultsmentioning

confidence: 99%

Photometry of asteroids (5141), (43032), (85953), (259221), and (363599) observed at Pic du Midi Observatory

et al. 2018

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These are the first results of an observational program devoted to the complete physical data of asteroids that could produce or feed meteoroid streams. Our results are based on the optical observation at Pic du Midi observatory in April 6–7, 2016 and January 17–18, 2018. We will present the light curve of asteroid (259221) 2003 BA21, associated with Daytime Sextantids (221 DSX) and November θ Aurigids (390 THA); the light curves and colors of asteroid (363599) 2004 FG11, associated with Daytime ζ Perseids (172 ZPE) as well as g − r and g − i; and the corresponding reflectances for the (85953) 1999 FK21, associated with Daytime ξ Sagittariids (100 XSA). We will also present the colors for two additional objects, namely, (5141) Tachibana and (43032) 1999 VR26.

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“…Now we consider a more realistic case (see, for instance, [3,11,28]): the N asteroids have different masses/diameters (still under the assumption that they have common densities δ) and may have different eccentricity. We will keep the assumption R i = R ∀i because the final estimate on ε will represent an upper bound also for a different average radius R i .…”

Section: Asteroids With Power-law Mass Distributionmentioning

confidence: 99%

“…Remarkably, our assumption about the radii distribution of the asteroids seems to be quite close to the observed one. In particular, the estimates obtained from observed data give a value of ν between 1.3 and 3 (see [28] and references therein). Again, the basic problem is to control the contributions of the collisions.…”

Section: Introductionmentioning

confidence: 99%

Lonely Planets and Lightweight Asteroids: A Statistical Mechanics Model for the Planetary Problem

Pinzari

Scoppola

Troiani

2021

Ann. Henri Poincaré

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In this paper we propose a notion of stability, which we call $$\varepsilon -N$$ ε - N -stability, for systems of particles interacting via Newton’s gravitational potential, and orbiting a much bigger object. For these systems the usual thermodynamical stability condition, ensuring the possibility to perform the thermodynamical limit, fails, but one can use as relevant parameter the maximum number of particles N that guarantees the $$\varepsilon -N$$ ε - N -stability. With some judicious but not particularly optimized estimates, borrowed from the classical theory of equilibrium statistical mechanics, we show that our model has a good fit with the data observed in the Solar System, and it gives a reasonable interpretation of some of its global properties.

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The kilometer-sized Main Belt asteroid population revealed bySpitzer

Cited by 40 publications

References 58 publications

The primordial nucleus of comet 67P/Churyumov-Gerasimenko

The primordial nucleus of comet 67P/Churyumov-Gerasimenko

Photometry of asteroids (5141), (43032), (85953), (259221), and (363599) observed at Pic du Midi Observatory

Lonely Planets and Lightweight Asteroids: A Statistical Mechanics Model for the Planetary Problem

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