New members of Datura family

Rosaev, A. E.; Plávalová, E.

doi:10.1016/j.pss.2017.01.017

Cited by 9 publications

(11 citation statements)

References 19 publications

(26 reference statements)

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“…Datura family.-Historically, a compact cluster of six small asteroids about (1270) Datura (thence the Datura family) was the first example of a very young family discovered . Its convenient location in the innermost part of the main belt, and large orbital eccentricity of ≃ 0.21 (thence low perihelia), allowed to quickly increase Datura's known population to the present-day census of 76 (see gradual steps in Vokrouhlický et al, 2009;Rosaev and Plávalová, 2017;Vokrouhlický et al, 2017a). Fig.…”

Section: Very Young Familiesmentioning

confidence: 99%

“…Finally, despite the compactness of the Datura family, the orbital history of some of its members happens to interact with a weak, high-order, mean motion resonance M9/16 with Mars (see already . Various aspects and illustrations of the resonant dynamics in M9/16 has been studied by Rosaev and Plávalová (2017) and more recently by Plávalová and Rosaev (2021). In general, such orbits present dynamical chaos effects that undermine their use for the family age determination based on regular-orbits convergence.…”

Section: Very Young Familiesmentioning

confidence: 99%

See 1 more Smart Citation

Asteroid Families: properties, recent advances and future opportunities

Novakovic,

Vokrouhlicky,

Spoto

et al. 2022

Preprint

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Collisions are one of the key processes shaping planetary systems. Asteroid families are outcomes of such collision still identifiable across our solar system. The families provide a unique view of catastrophic disruption phenomena and have been in the focus of planetary scientists for more than a century. Most of them are located in the main belt, a ring of asteroids between Mars and Jupiter. Here we review the basic properties of the families, discuss some recent advances, and anticipate future challenges. This review pays more attention to dynamic aspects such as family identification, age determination, and long-term evolution. The text, however, goes beyond that. Especially, we cover the details of young families that see the major advances in the last years, and we anticipate it will develop even faster in the future. We also discuss the relevance of asteroid families for water-ice content in the asteroid belt and our current knowledge on links between families and main-belt comets.

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Section: Very Young Familiesmentioning

confidence: 99%

Section: Very Young Familiesmentioning

confidence: 99%

Asteroid Families: properties, recent advances and future opportunities

Novakovic,

Vokrouhlicky,

Spoto

et al. 2022

Preprint

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“…Until recently, only seven members of the Datura family were known (Nesvorný et al , 2015Vokrouhlický et al 2009), all of them belonging to the so-called S-type of minor planets (Tholen 1984). According to our latest analyses (Rosaev & Plávalová 2017), however, three new members have to be included, and Vokrouhlický et al (2017) have reported on the existence of another seven. The total sum of known members of the Datura family might therefore be as high as 17 at the time of writing (see Table 1).…”

Section: Datura Family Main Factsmentioning

confidence: 99%

Dynamical effect of the 9:16 resonance with Mars on some Datura asteroids, including the pair Balam and 312497

Plávalová

Rosaev

2021

A&A

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Context. We studied the effect of the mean motion 9:16 resonance with Mars (9:16M) on the dynamics of the very young asteroid family Datura and the young pair (3749) Balam and (312497) 2009 BR60. Aims. We aim to understand the mechanism of dynamical interaction of the members of a family that are subjected to mean motion resonance in order to precisely estimate the age of an asteroid family or pair and to reconstruct their breakup processes. Methods. We calculated the expected (9:16M) resonance position, its boundaries, and multiplet fine structure and their time evolution under the effect of Mars orbit variations. We used the Lyapunov characteristic exponent and Euclid algorithm in our analytical calculations. We compared these results with backward numerical integrations of some Datura asteroids to check for consistency. Results. We explain the strong variations in the semi-major axis of some Datura asteroids as caused by the variations in the orbit of Mars. Using the Datura family as an example, we show that the distance from resonance may be a better measure of chaos than the widely accepted Lyapunov exponent. Additionally, we find that asteroid (3749) Balam exhibits the conspicuous effects of dynamical perturbations that are likely induced by the 9:16M resonance. Conclusions. Focusing on one of the most robust and well-established young asteroid families, the Datura family, we show that mean motion resonances play an important role as drivers of the dynamical evolution of asteroid families.

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“…This relatively young age makes this family a very interesting group that can provide important insights into largescale fragmentation and other physical processes that affect asteroids after their formation. Rosaev & Plávalová (2015) found three new members of the Datura family, and later Vokrouhlický et al (2017) presented a wealth of new data on that family: they extended its population to 17 members and two candidate members. They were able to derive spins for the six largest members and shapes of the four largest known members.…”

Section: The Datura Familymentioning

confidence: 99%

Interpretations of family size distributions: The Datura example

Henych¹,

Holsapple²

2018

Icarus

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Young asteroid families are unique sources of information about fragmentation physics and the structure of their parent bodies, since their physical properties have not changed much since their birth. Families have different properties such as age, size, taxonomy, collision severity and others, and understanding the effect of those properties on our observations of the size-frequency distribution (SFD) of family fragments can give us important insights into the hypervelocity collision processes at scales we cannot achieve in our laboratories. Here we take as an example the very young Datura family, with a small 8-km parent body, and compare its size distribution to other families, with both large and small parent bodies, and created by both catastrophic and cratering formation events. We conclude that most likely explanation for the shallower size distribution compared to larger families is a more pronounced observational bias because of its small size. Its size distribution is perfectly normal when its parent body size is taken into account. We also discuss some other possibilities. In addition, we study another common feature: an offset or "bump" in the distribution occurring for a few of the larger elements. We hypothesize that it can be explained by a newly described regime of cratering, "spall cratering", which controls the majority of impact craters on the surface of small asteroids like Datura.Comment: accepted for publication in Icarus; 21 pages, 10 figure

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New members of Datura family

Cited by 9 publications

References 19 publications

Asteroid Families: properties, recent advances and future opportunities

Asteroid Families: properties, recent advances and future opportunities

Dynamical effect of the 9:16 resonance with Mars on some Datura asteroids, including the pair Balam and 312497

Interpretations of family size distributions: The Datura example

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