Colors of dynamically associated asteroid pairs

Moskovitz, Nicholas

doi:10.1016/j.icarus.2012.07.011

Cited by 31 publications

(34 citation statements)

References 33 publications

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“…From their spectral observations, derived S and Sq/Q types for the primary and secondary, respectively. Their color indices are (V − R) 1 = 0.45 ± 0.02 (Moskovitz 2012) and (V − R) 2 = 0.444 ± 0.010 (our measurement). Using our derived mean absolute magnitude, we refined the WISE data (Masiero et al 2011) for the secondary (44612) and obtained D 2 = 2.0 ± 0.4 km and p V,2 = 0.22 ± 0.08.…”

Section: (2110) Moore-sitterly and (44612) 1999 Rp27supporting

confidence: 53%

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: (2110) Moore-sitterly and (44612) 1999 Rp27supporting

confidence: 53%

Asteroid pairs: A complex picture

Pravec

Fatka

Vokrouhlický

et al. 2019

Icarus

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“…Vokrouhlický and Nesvorný, 2009;Vokrouhlický, 2009;Pravec and Vokrouhlický, 2009;Žižka et al, 2016). A shared origin for asteroid pairs is supported by the similar photometric colors and/or spectral properties of the two components (Moskovitz, 2012;Duddy et al, 2013;Polishook et al, 2014a;Wolters et al, 2014). Several hundred candidate asteroid pair systems have been identified in the Main Belt (Pravec and Vokrouhlický, 2009).…”

Section: Introductionmentioning

confidence: 97%

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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“…In this scenario, NEOs with perihelia closer to the orbit of the Earth are more likely to produce fragments which is a reasonable hypothesis. Figure 11, left-hand panel, in which the groups with the highest significance have two-to-three members links directly to the topic of unbound asteroid pairs (see e.g Vokrouhlický & Nesvorný 2008;Pravec & Vokrouhlický 2009;Pravec et al 2010;Moskovitz 2012;Duddy et al 2013;Polishook et al 2014;Wolters et al 2014). Bona fide unbound asteroid pairs have been found in the main as-teroid belt.…”

Section: Discussionmentioning

confidence: 96%

Far from random: dynamical groupings among the NEO population

Marcos¹,

Marcos²

2015

Mon. Not. R. Astron. Soc.

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Among the near-Earth object (NEO) population there are comets and active asteroids which are sources of fragments that initially move together; in addition, some NEOs follow orbits temporarily trapped in a web of secular resonances. These facts contribute to increasing the risk of meteoroid strikes on Earth, making its proper quantification difficult. The identification and subsequent study of groups of small NEOs that appear to move in similar trajectories are necessary steps in improving our understanding of the impact risk associated with meteoroids. Here, we present results of a search for statistically significant dynamical groupings among the NEO population. Our Monte Carlo-based methodology recovers well-documented groupings like the Taurid Complex or the one resulting from the split comet 73P/SchwassmannWachmann 3, and new ones that may have been the source of past impacts. Among the most conspicuous are the Mjolnir and Ptah groups, perhaps the source of recent impact events like Almahata Sitta and Chelyabinsk, respectively. Meteoroid 2014 AA, that hit the Earth on 2014 January 2, could have its origin in a marginally significant grouping associated with Bennu. We find that most of the substructure present within the orbital domain of the NEOs is of resonant nature, probably induced by secular resonances and the Kozai mechanism that confine these objects into specific paths with well-defined perihelia.

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Colors of dynamically associated asteroid pairs

Cited by 31 publications

References 33 publications

Asteroid pairs: A complex picture

Asteroid pairs: A complex picture

A common origin for dynamically associated near-Earth asteroid pairs

Far from random: dynamical groupings among the NEO population

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