Size–frequency distributions of fragments from SPH/N-body simulations of asteroid impacts: Comparison with observed asteroid families

Durda, D. D.; Bottke, W. F.; Nesvorný, David; Enke, B. L.; Merline, W. J.; Asphaug, Erik; Richardson, D. C.

doi:10.1016/j.icarus.2006.09.013

Cited by 189 publications

(264 citation statements)

References 36 publications

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“…This KBO was then divided into a largest remnant containing half the mass and a population of smaller fragments containing the remaining mass of the original KBO. We did not perform any numerical simulations of the collisions, rather the family generation was informed by the numerical results of Durda et al (2007) and Z. M. Leinhardt & S. T. Stewart (2011, in preparation). The differential size distribution of the family was set as a power law with index q ranging from 4 to 6.…”

Section: Methodsmentioning

confidence: 99%

“…The asteroid belt includes identified collisional families that have formed by cratering impacts as well as those formed by catastrophic disruption (e.g., Durda et al 2007). One feature of those families formed in cratering events is that the largest impact fragment is considerably smaller in size than the target body.…”

Section: How Did Families Form?mentioning

confidence: 99%

“…No other KBO families have been confirmed (although one family was proposed and later retracted ;Chiang 2002;Chiang et al 2003), and additional collisional families in the Kuiper Belt are thought to be rare, or at least difficult to discover, for a number of reasons. Collisions typically result in a collection of objects with a velocity dispersion comparable to the parent body's escape velocity (e.g., Durda et al 2007). Orbital velocities in the Kuiper Belt are v kep 5 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

“…Such simulations have been performed for the asteroid belt (Durda et al 2007). However, in the asteroid belt, the size-velocity distribution of a family cannot be well constrained-with a few notable exceptions (e.g., )-because of the Yarkovsky effect: a thermal radiation force that causes small bodies to undergo semimajor axis drift as a function of their spin, orbit, and material properties .…”

Section: Introductionmentioning

confidence: 99%

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Identifying Collisional Families in the Kuiper Belt

Marcus

Ragozzine

Murray-Clay

et al. 2011

ApJ

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The identification and characterization of numerous collisional families-clusters of bodies with a common collisional origin-in the asteroid belt has added greatly to the understanding of asteroid belt formation and evolution. More recent study has also led to an appreciation of physical processes that had previously been neglected (e.g., the Yarkovsky effect). Collisions have certainly played an important role in the evolution of the Kuiper Belt as well, though only one collisional family has been identified in that region to date, around the dwarf planet Haumea. In this paper, we combine insights into collisional families from numerical simulations with the current observational constraints on the dynamical structure of the Kuiper Belt to investigate the ideal sizes and locations for identifying collisional families. We find that larger progenitors (r ∼ 500 km) result in more easily identifiable families, given the difficulty in identifying fragments of smaller progenitors in magnitude-limited surveys, despite their larger spread and less frequent occurrence. However, even these families do not stand out well from the background. Identifying families as statistical overdensities is much easier than characterizing families by distinguishing individual members from interlopers. Such identification seems promising, provided the background population is well known. In either case, families will also be much easier to study where the background population is small, i.e., at high inclinations. Overall, our results indicate that entirely different techniques for identifying families will be needed for the Kuiper Belt, and we provide some suggestions.

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Section: Methodsmentioning

confidence: 99%

Section: How Did Families Form?mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Identifying Collisional Families in the Kuiper Belt

Marcus

Ragozzine

Murray-Clay

et al. 2011

ApJ

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“…Interestingly, both values are much smaller than unity, with the following statistical values: m fragments /m Datura = 0.045 ± 0.009 and L fragments /L Datura = (1.03 ± 0.33) × 10 −3 . Therefore nominally, Datura-forming event should be classified as a cratering (e.g., Durda et al 2007). Additional circumstance here is that the largest remnant holds not only most of the mass of the parent body, but it also retained most of its angular momentum.…”

Section: Debiased Datura-family Populationmentioning

confidence: 99%

The young Datura asteroid family

Vokrouhlický

Pravec

Ďurech

et al. 2017

A&A

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Context. Asteroid families are the outcomes of disruption or cratering events on a size and energy scales that are not reproducible in laboratory experiments. Overall structure, as well as properties of individual members, in the old families could have been changed since their formation. Therefore young families preserve best the characteristics of the initial event. Aims. We study the most suitable known asteroid family with an age of less than 1 Myr, the Datura family. We aim (i) to obtain information about rotation state and shape of the largest members in the family; and (ii) to constrain its debiased population down to couple of hundreds of meters in size. Methods. We have analyzed the up-to-date catalog of orbital elements of main belt asteroids. We evaluated the detection efficiency of Catalina Sky Survey (CSS) in regard to detections of members in the Datura family, and we have used our photometric observations and lightcurve inversion methods to determine the rotation states and shapes of the largest members of the family. Results. We determined rotation periods of the seven largest members of the Datura family, and we also derived accurate mean absolute magnitudes for six of them. Except for the largest fragment (1270) Datura, the asteroids tend to have long rotation periods and large amplitude of the lightcurve, witnessing an elongated shape. For the four largest asteroids, our observations allow us to resolve rotation pole and a rough shape. All of them are prograde-rotating and have the latitude of the rotation pole >50 • . Our search in orbital catalogs resulted in the discovery of many small, sub-kilometer members of the Datura family. Using the CSS detection efficiency, we inverted this information into the debiased population of Datura family members. We show that the mass and angular momentum content in small fragments is negligible compared to the largest fragment (1270) Datura. These findings may help to constrain the formation mechanism of the family.

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Creation, detection, and evolution of Jupiter Trojan families

Karlsson

2011

Astron Nachr

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An investigation is carried out looking at correlations between the orbital elements of collisional targets and projectiles, estimating the number of interlopers in Trojan collisional families, and at the possibility of determining the ages of the Jupiter Trojan families by orbital integration. Real Trojans are integrated and close encounters are recorded in order to evaluate collisional circumstances between Trojans. Fictitious collisional families are created and integrated for 10 MJyr (million Julian years) forward in time and back again to the time of the collision in order to check the performance of the integrator, and the behaviour of the fictitious collisional fragments. Proper elements are calculated for the detection of family clustering using the hierarchically clustering method. This method presents little difficulty finding fictitious families in the Trojan swarms even in areas with densely populated backgrounds. However, even when the background is relatively sparse in objects, several interlopers can be connected to the family at velocity differences below 100 m s −1 . On the other hand, in densely populated backgrounds the contamination of interlopers should be less than 30 %. Providing gravity is the only significant force acting on the Trojans and resonance effects are weak, the shape the collision fragments create in the proper element space are preserved on the GJyr scale, and collisions can be tracked with orbital integrations for ages of at least 100 MJyr. However, the shape of artificial families does not correspond to suggested real families. This points to the need of including non-gravitational forces such as the Yarkovsky effect in order to simulate the family evolution. As a consequence age determination by orbital integration might be severely restricted and previous investigations involving long term orbital integrations might have to be recalculated.

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Size–frequency distributions of fragments from SPH/N-body simulations of asteroid impacts: Comparison with observed asteroid families

Cited by 189 publications

References 36 publications

Identifying Collisional Families in the Kuiper Belt

Identifying Collisional Families in the Kuiper Belt

The young Datura asteroid family

Creation, detection, and evolution of Jupiter Trojan families

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