Karin cluster formation by asteroid impact

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

doi:10.1016/j.icarus.2006.03.008

Cited by 69 publications

(102 citation statements)

References 49 publications

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“…With six members on reasonably well-constrained orbits (Table 1), we are able to reconstruct the past configuration of this asteroid cluster to higher accuracy than before. Surprisingly, we find possible age solutions that are older than the value of ∼450 kyr previously reported by Nesvorný et al (2006b).…”

Section: Introductioncontrasting

confidence: 61%

“…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%

“…The discovery of very young asteroid clusters (e.g., Nesvorný et al 2006b;Pravec & Vokrouhlický 2009) started a new phase in the analysis of the asteroid families. This is because we have become aware of many dynamical and physical processes that modify the configuration and the observable parameters of their individual members with time.…”

Section: Introductionmentioning

confidence: 99%

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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: Introductioncontrasting

confidence: 61%

Section: Rotation Period For (90265) 2003 Cl5mentioning

confidence: 86%

Section: Introductionmentioning

confidence: 99%

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Datura family: the 2009 update

Vokrouhlický¹,

Ďurech²,

Michałowski

et al. 2009

A&A

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“…6, is rather shallow. Compare it, for instance, with the steep size distribution of the somewhat older Karin family (e.g., Nesvorný et al 2006a). In quantitative terms we note that we have basically two solutions for Datura's size distribution (see Figs.…”

Section: Discussionmentioning

confidence: 98%

“…This 5.75 Myr old family was formed when a 5.8 km size impactor blasted a 33 km size parent body by hitting it at 5−6 km s −1 velocity producing A&A 598, A91 (2017) about hundred fragments larger than 2.5 km (e.g., Nesvorný et al 2006a). A couple of similar, but less well characterized families, of this category were discovered in the subsequent years (e.g., Nesvorný et al 2015).…”

Section: Introductionmentioning

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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Dynamic Sources of Contemporary Hazard from Meteoroids and Small Asteroids

Trigo-Rodríguez

Williams

2016

Astrophysics and Space Science Proceedings

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Karin cluster formation by asteroid impact

Cited by 69 publications

References 49 publications

Datura family: the 2009 update

Datura family: the 2009 update

The young Datura asteroid family

Dynamic Sources of Contemporary Hazard from Meteoroids and Small Asteroids

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