Erratum to “Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion” [Icarus 179 (2005) 63–94]

Bottke, W. F.; Durda, D. D.; Nesvorný, David; Jedicke, Robert; Morbidelli, Alessandro; Vokrouhlický, D.; Levison, Harold F.

doi:10.1016/j.icarus.2006.02.014

Cited by 114 publications

(169 citation statements)

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“…This result probably implies that the disrupted body was small, perhaps only several kilometers across, such that the largest fragments produced by the breakup have sizes below the current detection limit. According to Bottke et al (2005), a 1 km diameter asteroid disrupts in the main belt every $100 yr and a 10 km diameter asteroid every $100 kyr.…”

Section: Discussionmentioning

confidence: 99%

Candidates for Asteroid Dust Trails

et al. 2006

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The contribution of different sources to the circumsolar dust cloud (known as the zodiacal cloud) can be deduced from diagnostic observations. We used the Spitzer Space Telescope to observe the diffuse thermal emission of the zodiacal cloud near the ecliptic. Several structures were identified in these observations, including previously known asteroid dust bands, which are thought to have been produced by recent asteroid collisions, and cometary trails. Interestingly, two of the detected dust trails, denoted t1 and t2 here, cannot be linked to any known comet. Trails t1 and t2 represent a much larger integrated brightness than all known cometary trails combined and may therefore be major contributors to the circumsolar dust cloud. We used our Spitzer observations to determine the orbits of these trails and were able to link them to two (''orphan'' or type II) trails that were discovered by the Infrared Astronomical Satellite (IRAS ) in 1983. The orbits of trails t1 and t2 that we determined by combining the Spitzer and IRAS data have semimajor axes, eccentricities, and inclinations like those of the main-belt asteroids. We therefore propose that trails t1 and t2 were produced by very recent (P100 kyr old) collisional breakups of small, P10 km diameter main-belt asteroids.

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Section: Discussionmentioning

confidence: 99%

Candidates for Asteroid Dust Trails

et al. 2006

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“…What is an approximate size d disrupt of a projectile necessary to disrupt the parent body of the Schubart family? Using from Bottke et al (2005): and substituting Q * D = 10 5 J kg −1 for the strength (somewhat lower than that of basaltic objects to accommodate the assumed C/X spectral type; e.g. Kenyon et al 2008 and references therein), V imp = 4.78 km s −1 for the typical impact velocity (see Dahlgren 1998) and D target ≃ 130 km, we obtain d disrupt ≃ 25 km.…”

Section: Collisional Families Among Hilda Asteroidsmentioning

confidence: 93%

Asteroid families in the first-order resonances with Jupiter

Brož¹,

Vokrouhlický²

2008

Monthly Notices of the Royal Astronomical Society

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Asteroids residing in the first‐order mean motion resonances with Jupiter hold important information about the processes that set the final architecture of giant planets. Here, we revise current populations of objects in the J2/1 (Hecuba‐gap group), J3/2 (Hilda group) and J4/3 (Thule group) resonances. The number of multi‐opposition asteroids found is 274 for J2/1, 1197 for J3/2 and three for J4/3. By discovering a second and third object in the J4/3 resonance (186024) 2001 QG207 and (185290) 2006 UB219, this population becomes a real group rather than a single object. Using both hierarchical clustering technique and colour identification, we characterize a collisionally born asteroid family around the largest object (1911) Schubart in the J3/2 resonance. There is also a looser cluster around the largest asteroid (153) Hilda. Using N‐body numerical simulations we prove that the Yarkovsky effect (infrared thermal emission from the surface of asteroids) causes a systematic drift in eccentricity for resonant asteroids, while their semimajor axis is almost fixed due to the strong coupling with Jupiter. This is a different mechanism from main belt families, where the Yarkovsky drift affects basically the semimajor axis. We use the eccentricity evolution to determine the following ages: (1.7 ± 0.7) Gyr for the Schubart family and ≳4 Gyr for the Hilda family. We also find that collisionally born clusters in the J2/1 resonance would efficiently dynamically disperse. The steep size distribution of the stable population inside this resonance could thus make sense if most of these bodies are fragments from an event older than ≃1 Gyr. Finally, we test stability of resonant populations during Jupiter's and Saturn's crossing of their mutual mean motion resonances. In particular, we find primordial objects in the J3/2 resonance were efficiently removed from their orbits when Jupiter and Saturn crossed their 1:2 mean motion resonance.

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“…Current observational estimates on the number of NEAs with diameter of the order of 10 m range from 10 7 to about 5 × 10 7 (Brown et al 2002; Ivanov et al 2002; Bottke et al 2005). Suppose that only 5–10 per cent of these are on low‐eccentricity orbits (Rabinowitz 1994), then we have about 10 5 such objects.…”

Section: Originmentioning

confidence: 99%

Asteroids on Earth-like orbits and their origin

Brasser

Wiegert

2008

Monthly Notices RAS

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The orbit of 1991 VG and a set of other asteroids whose orbits are very similar to that of the Earth have been examined. Its origin has been speculated to be a returning spacecraft, lunar ejecta or a low‐inclination Amor‐ or Apollo‐class object. The latter is arguably the more likely source, which has been investigated here. The impact probability for these objects has been calculated, and while it is larger than that of a typical near‐Earth asteroid (NEA), it is still less than 1:200 000 over the next 5000 yr. In addition, the probability of an NEA ever ending up on an Earth‐like orbit has been obtained from numerical simulations and turned out to be about 1:20 000, making this a rare class of objects. The typical time spent in this state is about 10 000 yr, much less than the typical NEA lifetime of 10 Myr.

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Erratum to “Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion” [Icarus 179 (2005) 63–94]

Cited by 114 publications

References 0 publications

Candidates for Asteroid Dust Trails

Candidates for Asteroid Dust Trails

Asteroid families in the first-order resonances with Jupiter

Asteroids on Earth-like orbits and their origin

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