A Study of Asteroid Families and Streams by Computer Techniques

Lindblad, B. A.; Southworth, R. B.

doi:10.1017/s0252921100089181

Cited by 15 publications

(6 citation statements)

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“…We use the D SH metric in its original form because it has an established pedigree (e.g. searching for parent comets of meteor streams) that has been used to successfully identify members of known meteor streams (Southworth & Hawkins 1963, Sekanina 1970) and main belt asteroid families (Lindblad & Southworth 1971).…”

Section: The Southworth-hawkins D-criterionmentioning

confidence: 99%

Searching for the first near-Earth object family

Schunová

Granvik

Jedicke

et al. 2012

Icarus

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a b s t r a c tWe report on our search for genetically related asteroids amongst the near-Earth object (NEO) population-families of NEOs akin to the well known main belt asteroid families. We used the technique proposed by Fu et al. (Fu, H., Jedicke, R., Durda, D.D., Fevig, R. Binzel, R.P. [2005]. Icarus 178(2), 434-449) supplemented with a detailed analysis of the statistical significance of the detected clusters. Their significance was assessed by comparison to identical searches performed on 1000 'fuzzy-real' NEO orbit distribution models that we developed for this purpose. The family-free 'fuzzy-real' NEO models maintain both the micro and macro distribution of five orbital elements (ignoring the mean anomaly). Three clusters were identified that contain four or more NEOs but none of them are statistically significant at P 3r. The most statistically significant cluster at the $ 2r level contains four objects with H < 20 and all members have long observational arcs and concomitant good orbital elements. Despite the low statistical significance we performed several other tests on the cluster to determine if it is likely a genetic family. The tests included examining the cluster's taxonomy, size-frequency distribution, consistency with a familyforming event during tidal disruption in a close approach to Mars, and whether it is detectable in a proper element cluster search. None of these tests exclude the possibility that the cluster is a family but neither do they confirm the hypothesis. We conclude that we have not identified any NEO families.Published by Elsevier Inc.

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Section: The Southworth-hawkins D-criterionmentioning

confidence: 99%

Searching for the first near-Earth object family

Schunová

Granvik

Jedicke

et al. 2012

Icarus

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“…So, it is sufficient to find concentrations in another two orbital elements (angular elements -the longitude of the perihelion and the longitude of the ascending node) in asteroid families for the purpose of finding orbital clustering. Such orbital clusterings were found by AlfvCn (1969) and subsequently by Arnold (1969) and Lindblad and Southworth (1971). Flora A found by AlfvCn is the most marked orbital clustering.…”

Section: Introductionmentioning

confidence: 71%

Asteroidal jet-stream Flora A

Klačka

1991

Earth Moon Planet

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“…Brouwer (1951) used an enhanced Lagrange-type analytical solution of the linear secular perturbation equations and the major planet theory by Brouwer and Van Woerkom (1950) to produce proper elements for all asteroids numbered at that time; his procedure and results were rather advanced with respect to the previous ones and therefore they were used for quite some time (cf. Anders, 1965;Arnold, 1969;Van Houten et al, 1970;Lindblad and Southworth, 1971 Williams (1979) and by Williams and Hierath (1987), and are sometimes still in use (they can also be found in Williams, 1989). The positions of the surfaces of the linear secular resonances, which are the most important because they bound the main asteroid belt and open large gaps in the distribution of asteroids, were determined using this theory by Williams and Faulkner (1981).…”

Section: Theories and Methods For Computation Of Proper Elementsmentioning

confidence: 99%

“…Brouwer (1951) used an enhanced Lagrange-type analytical solution of the linear secular perturbation equations and the major planet theory by Brouwer and Van Woerkom (1950) to produce proper elements for all asteroids numbered at that time; his procedure and results were rather advanced with respect to the previous ones and therefore they were used for quite some time (cf. Anders, 1965;Arnold, 1969;Van Houten et al, 1970;Lindblad and Southworth, 1971 when Williams (1969) developed a new semianalytic theory, which used no expansion of the perturbing function in eccentricity and inclination of the asteroid, and thus provided results of about the same accuracy regardless of e, I. Proper elements computed by means of this theory have been published by Williams (1979) and by Williams and Hierath (1987), and are sometimes still in use (they can also be found in Williams, 1989).…”

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confidence: 99%

Asteroid Proper Elements: The Big Picture

Knežević

Milani²

1994

Symp. - Int. Astron. Union

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Abstract. Four perturbation theories presently used to compute asteroid proper elements are reviewed, and their results are briefly discussed (Milani and Knezevic, 1990, for low to moderate eccentricity/inclination main belt objects; Lemaitre and Morbidelli, 1994, for high e, J objects; Milani, 1993, for Trojans;Schubart, 1982, 1991. The most important recent improvements are described, in particular those pertaining to the upgrades of the previous analytic and semianalytic solutions. The dynamical structure of the asteroid main belt, as defined by the low order mean motion resonances and by linear and nonlinear secular resonances, is considered from the point of view of the effects of these resonances on the accuracy and/or reliability of the computation of proper elements and on the reliability of the identification of asteroid families. What are the proper elements and what they are used for?Asteroid proper elements are quasi-integrals of motion, stable over very long intervals of time; they represent a sort of "average" characteristics of motion in the sense that they result from a procedure of elimination of short-and long-periodic perturbations. The proper elements are used for two main purposes : (i) they serve as parameters for classification of asteroids into families; (ii) they are employed for studies of the dynamical structure of the asteroid belt.Asteroid families are groupings of asteroids in the phase space of orbital elements. They were formed by catastrophic breakup of parent bodies, at unknown times in the remote past, and under circumstances (such as geometry of collision, physical properties of the parents, etc.) that are not yet fully understood. The parent body at the breakup might have had osculating elements significantly different from the corresponding proper values; since we do not know the epoch of the collision, the proper elements (due to their constancy in time) become the only tool to reliably recognize families, in particular the small ones consisting of a few members. Until recently, the very identification of the families and their memberships were not very reliable : the proper elements used for this identification were not accurate enough, and/or the classification methods suffered from subjectivity, biases, uncertainties due to insufficient data, etc. The situation is now greatly improved in both respects; the review of the current state of the art regarding proper elements and family classification is the subject of this and some other papers in this book (see e.g. Zappalà and Cellino, Milani, Burbine and Binzel).The differences of proper orbital elements between family members are related to their relative velocities, averaged over the unknown quantity, the age of the family. In order to reliably recognize the families, the changes in the proper elementsover time spans of the order of the family ages-must not exceed an amount given by the typical relative velocities of the family members. The relative velocities of family members are known to be of the order of 100 m/s; f...

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A Study of Asteroid Families and Streams by Computer Techniques

Cited by 15 publications

References 6 publications

Searching for the first near-Earth object family

Searching for the first near-Earth object family

Asteroidal jet-stream Flora A

Asteroid Proper Elements: The Big Picture

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