The formation of asteroid satellites in large impacts: results from numerical simulations

Durda, D. D.; Bottke, W. F.; Enke, B. L.; Merline, W. J.; Asphaug, Erik; Richardson, D. C.; Leinhardt, Z. M.

doi:10.1016/j.icarus.2004.04.003

Cited by 130 publications

(146 citation statements)

References 31 publications

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“…We note that the hydrocode simulations of asteroid fragmentation do predict large fraction of binary fragments, the so-called escaping ejecta binaries (e.g., Durda et al 2004;Nesvorný et al 2006b;Richardson et al 2009). However, it seems that (90265) 2003 CL5 being a bi-lobed object (perhaps a failed binary) would challenge several current models.…”

Section: Rotation Period For (90265) 2003 Cl5mentioning

confidence: 86%

Datura family: the 2009 update

Vokrouhlický¹,

Ďurech²,

Michałowski

et al. 2009

A&A

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Context. Research of asteroid families has been recently refreshed by the discovery of very young ones. These families are of great interest because they represent the product of their parent body fragmentation before orbital and physical evolutionary processes can change them. A cluster of seven objects around the largest body (1270) Datura is of particular interest because it has enough known members and resides in the inner part of the main asteroid belt, facilitating observations. Aims. We carried out photometric observations of the two largest members of the Datura family -asteroids (1270) Datura and (90265) 2003 CL5 -with the goal of inferring their physical parameters. We also used numerous astrometric observations of Datura-family members in the past few years to revisit the age of this cluster. Methods. We performed numerous photometric observations of (1270) Datura over several oppositions. We then used the lightcurve inversion method to determine the spin state and shape of this asteroid. In the case of (90265) 2003 CL5, for which only limited lightcurve data have been acquired so far, we used Fourier analysis to determine the synodic rotation period during the 2008 apparition. We also used backward numerical integration of the improved orbits of Datura family members to reduce uncertainty in its age. Results. We determined the rotation state of (1270) Datura, the largest member of its own family. Its major properties are a short rotation period of ∼3.36 h and small obliquity, which, however, exhibits ∼±15 • excursions because of a forced Cassini state of the proper nodal frequency. Any possible initial non-principal rotation state has probably been damped and the asteroid rotates about the shortest axis of the inertia tensor. Its global shape, although convex in our representation, may reflect regions related to the excavation of the family members from the parent body surface. Interestingly, the second largest member of the Datura family -(90265) 2003 CL5 -appears to be very slow rotator with the rotation period ∼24 h. The large amplitude of its rotation curve suggests that its shape is extremely elongated, possibly bi-lobed. Improved orbits of the family members allow us to re-determine the possible age of this family. We find an age that is slightly older than previously reported. Using a conservative approach, we obtain an age in the 450 to 600 kyr range. With strengthened, but plausible, conditions, we find that the current data may support an age of 530±20 kyr. Further astrometric and photometric observations of the Datura cluster members are needed to determine its age more accurately.

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Section: Rotation Period For (90265) 2003 Cl5mentioning

confidence: 86%

Datura family: the 2009 update

Vokrouhlický¹,

Ďurech²,

Michałowski

et al. 2009

A&A

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“…Various models have been proposed to explain the formation of binary and multiple systems, such as the L 3 mechanism by Goldreich et al (2002), the L 2 s mechanism by Goldreich et al (2002), the chaos-assisted capture by Astakhov et al (2005), the collisional model by Durda et al (2004), the hybrid model by Weidenschilling (2002), the gravitational collapse by Nesvorný et al (2010), and the rotational fission model by Ortiz et al (2012b). A complete review of some of these mechanisms can be found in Noll et al (2008).…”

Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 99%

Rotational properties of the binary and non-binary populations in the trans-Neptunian belt

Thirouin

Noll

Ortiz

et al. 2014

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We present results for the short-term variability of binary trans-Neptunian objects (BTNOs). We performed CCD photometric observations using the 3.58 m Telescopio Nazionale Galileo (TNG), the 1.5 m Sierra Nevada Observatory (OSN) telescope, and the 1.23 m Centro Astronómico Hispano Alemán (CAHA) telescope at Calar Alto Observatory. We present results based on five years of observations and report the short-term variability of six BTNOs. Our sample contains three classical objects: (174567) We also derived some physical properties from their light curves, such as density, primary and secondary sizes, and albedo. We compiled and analyzed a vast light curve database for TNOs including centaurs to determine the light-curve amplitude and spin frequency distributions for the binary and non-binary populations. The mean rotational periods, from the Maxwellian fits to the frequency distributions, are 8.63 ± 0.52 h for the entire sample, 8.37 ± 0.58 h for the sample without the binary population, and 10.11 ± 1.19 h for the binary population alone. Because the centaurs are collisionally more evolved, their rotational periods might not be so primordial. We computed a mean rotational period, from the Maxwellian fit, of 8.86 ± 0.58 h for the sample without the centaur population, and of 8.64 ± 0.67 h considering a sample without the binary and the centaur populations. According to this analysis, regular TNOs spin faster than binaries, which is compatible with the tidal interaction of the binaries. Finally, we examined possible formation models for several systems studied in this work and by our team in previous papers.

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“…The apparent orientation of Elektra generated with the pole I solution is remarquably similar to the observations (see Table 4a). The observations recorded on Jan. 5, 2004 andJan. 15, 2005 are clearly different in appearance than the pole II model.…”

Section: Size and Shape Of (130) Elektra's Primarymentioning

confidence: 99%

“…µQ ~10 10 is the best guess for this parameter product considering Q~100 as measured for Phobos by Yoder (1982) and µ ~10 8 N m -2 a typical value for a moderately fractured asteroid. Durda et al (2004) do not discuss the value of a i in their SPH simulations of collisions and formation of moonlet binary asteroids, but we can neglect the term (a i /R p ) 13/2 since (a f /R p ) ~ 10 from our analysis in the equation 4 and directly invert it to estimate the time scale τ. We derive an approximate age for (130) Elektra and (283) Emma of greater than 4.5 billion years and ~10 million years respectively (see Fig.…”

Section: Time Scale For Semi-major Axesmentioning

confidence: 99%

“…At the time of writing, more than sixty systems have been imaged, but the number of suspected binary asteroids is significantly higher (~145) since many of them display mutual event signatures (Behrend et al 2006, Descamps et al 2007) and/or multi-period components (Pravec and Harris, 2007) in their lightcurves. Despite recent simulations involving catastrophic collisions (Durda et al 2004), fission via the YORP effect (Cuk et al 2005), and split due to tidal effect with a major planet (Walsh and Richardson, 2006) among others, the formation of most of these multiple asteroid systems is not yet understood. Insights into these binary systems, such as the orbital parameters of the satellite, the size and shape of the components of the system, the nature of their surface, their bulk density and distribution of materials in their interior could provide a better understanding of how these multiple asteroidal systems formed.…”

Section: Introductionmentioning

confidence: 99%

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