Orbital similarity functions - application to asteroid pairs

Rożek, A.; Breiter, S.; Jopek, T. J.

doi:10.1111/j.1365-2966.2010.17967.x

Cited by 18 publications

(18 citation statements)

References 15 publications

(46 reference statements)

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“…Following Zappalà et al (1990) and Pravec and Vokrouhlický (2009), we used k a = 5/4, k e = k i = 2 and k ̟ = k Ω = 10 −4 . The distance d mean between two asteroid orbits is an approximate gauge for the relative velocity of the asteroids at close encounter (see Rożek et al 2011 for explicit tests and a comparison with other metric functions used in meteoritics). For most asteroid pairs, it is in the range from a few 10 −1 to a few 10 m/s.…”

Section: Pair Identification and Age Estimationmentioning

confidence: 99%

Asteroid pairs: A complex picture

Pravec

Fatka

Vokrouhlický

et al. 2019

Icarus

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We studied a sample of 93 asteroid pairs, i.e., pairs of genetically related asteroids that are on highly similar heliocentric orbits. We estimated times elapsed since separation of pair members (i.e., pair age) that are between 7 × 10 3 yr and a few 10 6 yr. With photometric observations, we derived the rotation periods P 1 for all the primaries (i.e., the larger members of asteroid pairs) and a sample of secondaries (the smaller pair members). We derived the absolute magnitude differences of the studied asteroid pairs that provide their mass ratios q. For a part of the studied pairs, we refined their WISE geometric albedos and collected or estimated their taxonomic classifications. For 17 asteroid pairs, we also determined their pole positions. In two pairs where we obtained the spin poles for both pair components, we saw the same sense of rotation for both components and constrained the angles between their original spin vectors at the time of their separation. We found that the primaries of 13 asteroid pairs in our sample are actually binary or triple systems, i.e., they have one or two bound, orbiting secondaries (satellites). As a by-product, we found also 3 new young asteroid clusters (each of them consisting of three known asteroids on highly similar heliocentric orbits). We compared the obtained asteroid pair data with theoretical predictions and discussed their implications. We found that 86 of the 93 studied asteroid pairs follow the trend of primary rotation period vs mass ratio that was found by Pravec et al. (2010). Of the 7 outliers, 3 appear insignificant (may be due to our uncertain or incomplete knowledge of the three pairs), but 4 are high mass ratio pairs that were unpredicted by the theory of asteroid pair formation by rotational fission. We discuss a (remotely) possible way that they could be created by rotational fission of flattened parent bodies followed by re-shaping of the formed components. The 13 asteroid pairs with binary primaries are particularly interesting systems that place important constraints on formation and evolution of asteroid pairs. We present two hypotheses for their formation: The asteroid pairs having both bound and unbound secondaries could be "failed asteroid clusters", or they could be formed by a cascade primary spin fission process. Further studies are needed to reveal which of these two hypotheses for formation of the paired binary systems is real.

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Section: Pair Identification and Age Estimationmentioning

confidence: 99%

Asteroid pairs: A complex picture

Pravec

Fatka

Vokrouhlický

et al. 2019

Icarus

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“…kyr (Rożek et al, 2011). Though there are known issues with the various implementations of D criteria (e.g.…”

Section: Pair Proximitymentioning

confidence: 99%

A common origin for dynamically associated near-Earth asteroid pairs

Moskovitz

Fatka

Farnocchia

et al. 2019

Icarus

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identified and studied for over a decade, very few pair systems have been identified in the near-Earth asteroid population. We present data and analysis that supports the existence of two genetically related pairs in near-Earth space. The members of the individual systems, 2015 EE7 -2015 FP124 and 2017 SN16 -2018 RY7, are found to be of the same spectral taxonomic class, and both pairs are interpreted to have volatile-poor compositions. In conjunction with dynamical arguments, this suggests that these two systems formed via YORP spin-up and/or dissociation of a binary precursor. Backwards orbital integrations suggest a separation age of < 10 kyr for the pair 2017 SN16 -2018 RY7, making these objects amongst the youngest multiple asteroid systems known to date. A unique separation age was not realized for 2015 EE7 -2015 FP124 due to large uncertainties associated with these objects' orbits. Determining the ages of such young pairs is of great value for testing models of space weathering and asteroid spin-state evolution. As the NEO catalog continues to grow with current and future discovery surveys, it is expected that more NEO pairs will be found, thus providing an ideal laboratory for studying time dependent evolutionary processes that are relevant to asteroids throughout the Solar System.

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“…Vokrouhlický & Nesvorný (2008); Rożek et al (2011) searched for Main Belt asteroid pairs suspected of having a common origin. ?…”

Section: Introductionmentioning

confidence: 99%

Probability of coincidental similarity among the orbits of small bodies – I. Pairing

Jopek

Bronikowska

2017

Planetary and Space Science

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Probability of coincidental clustering among the orbits of comets, asteroids and meteoroids depends on many factors like: the size of the orbital sample searched for clusters or the size of the identified group, it is different for groups of 2,3,4, ... members. Probability of coincidental clustering is assessed by the numerical simulation, therefore, it depends also on the method used for the synthetic orbits generation.We tested the impact of some of these factors. For a given size of the orbital sample we have assessed probability of random pairing among several orbital populations of different sizes. We have found how these probabilities vary with the size of the orbital samples.Finally, keeping fixed size of the orbital sample we have shown that the probability of random pairing can be significantly different for the orbital samples obtained by different observation techniques. Also for the user convenience we have obtained several formulae which, for given size of the orbital sample, one can use to calculate the similarity threshold corresponding to the small value of the probability of coincidental similarity among two orbits.

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Orbital similarity functions - application to asteroid pairs

Cited by 18 publications

References 15 publications

Asteroid pairs: A complex picture

Asteroid pairs: A complex picture

A common origin for dynamically associated near-Earth asteroid pairs

Probability of coincidental similarity among the orbits of small bodies – I. Pairing

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