Deficit of primitive compositions in binary asteroids and pairs

Minker, K; Carry, B.

doi:10.1051/0004-6361/202245538

Cited by 6 publications

(2 citation statements)

References 78 publications

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“…Beyond considering the internal structure, the evolution of a rubble-pile body after reaching its spin limit is also heavily influenced by numerous other factors, such as shape and surface morphology (Hirabayashi & Scheeres 2019;Hirabayashi et al 2020;Zhang et al 2022). This complexity implies that the surface failure conditions could vary across different bodies, which determines why certain asteroids evolved into binary systems while others did not, and could play some role in the apparent deficit of small binaries and pairs among primitive asteroid types relative to silicate-rich bodies (Minker & Carry 2023). In Section 2.1, to validate the assumed binary formation scenario for Didymos, we will present an SSDEM simulation example to showcase the feasibility of Didymos's mass-shedding failure behavior under reasonable conditions.…”

Section: Yorp Spin-up and Mass Sheddingmentioning

confidence: 99%

Direct N-body Simulations of Satellite Formation around Small Asteroids: Insights from DART’s Encounter with the Didymos System

Agrusa,

Zhang,

Richardson

et al. 2024

Planet. Sci. J.

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We explore binary asteroid formation by spin-up and rotational disruption considering the NASA DART mission's encounter with the Didymos–Dimorphos binary, which was the first small binary visited by a spacecraft. Using a suite of N-body simulations, we follow the gravitational accumulation of a satellite from meter-sized particles following a mass-shedding event from a rapidly rotating primary. The satellite’s formation is chaotic, as it undergoes a series of collisions, mergers, and close gravitational encounters with other moonlets, leading to a wide range of outcomes in terms of the satellite's mass, shape, orbit, and rotation state. We find that a Dimorphos-like satellite can form rapidly, in a matter of days, following a realistic mass-shedding event in which only ∼2%–3% of the primary's mass is shed. Satellites can form in synchronous rotation due to their formation near the Roche limit. There is a strong preference for forming prolate (elongated) satellites, although some simulations result in oblate spheroids like Dimorphos. The distribution of simulated secondary shapes is broadly consistent with other binary systems measured through radar or lightcurves. Unless Dimorphos's shape is an outlier, and considering the observational bias against lightcurve-based determination of secondary elongations for oblate bodies, we suggest there could be a significant population of oblate secondaries. If these satellites initially form with elongated shapes, a yet-unidentified pathway is needed to explain how they become oblate. Finally, we show that this chaotic formation pathway occasionally forms asteroid pairs and stable triples, including coorbital satellites and satellites in mean-motion resonances.

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Section: Yorp Spin-up and Mass Sheddingmentioning

confidence: 99%

Direct N-body Simulations of Satellite Formation around Small Asteroids: Insights from DART’s Encounter with the Didymos System

Agrusa,

Zhang,

Richardson

et al. 2024

Planet. Sci. J.

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“…Many fast-rotating asteroids are top-shaped, which Cheng et al (2021) is explained to be the result of the rotational instability. Moreover, a number of the primary of binary asteroids systems are found to be top-shaped, fast rotating, and fragile (Sánchez & Scheeres 2014;Minker & Carry 2023). This may indicate a secondary forming from the prior YORP-induced mass shedding (Walsh et al 2008;Hyodo & Sugiura 2022).…”

Section: Introductionmentioning

confidence: 97%

Regolith resurfacing and shedding on spinning spheroidal asteroids: Dependence on the surface mechanical properties

Dai,

Yu,

Cheng

et al. 2024

A&A

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The Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect has been shown to effectively alter the rotational status of asteroids. The spin-up of the asteroid leads to surface instability and eventually triggers regolith failure, followed by landslide and mass shedding on the asteroid's surface. We explore the dynamics of the rotation-induced resurfacing and shedding, paying special attention to the dependence of post-shedding evolution on regolith mechanical properties, such as cohesion. We propose a qualitative semi-analytical model to explore the post-failure dynamics of a fast-rotating asteroid. We also consider the interaction between the surface mass rearrangement and the asteroid’s spin status. We used our model to investigate the surface region where the failure occurs, as well as the total mass shed from the surface and the spin-down of the asteroid in this process. Based on our model, all the possible avalanche events following a regolith failure can be classified into four basic types: resurfacing (ReS), shedding and resurfacing (S ReS), shed and bound (S-Bound), and shedding and escaping (S-Escp). Their corresponding regions in the parameter space are illustrated in this work. Our results show that although the regolith cohesion is very small ($ 1-2$Pa), cohesion plays an important role in the onset of the avalanche. Moreover, our model qualitatively reconstructs the links between the regolith’s properties and the dynamical fates of the shed material. The timescale of YORP-induced shedding events is also discussed in this work.

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Binary asteroid candidates in Gaia DR3 astrometry

Liberato,

Tanga,

Mary

et al. 2024

A&A

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Asteroids with companions constitute an excellent sample for studying the collisional and dynamical evolution of minor planets. The currently known binary population were discovered by different complementary techniques that produce, for the moment, a strongly biased distribution, especially in a range of intermediate asteroid sizes (approx 20 to 100 km) where both mutual photometric events and high-resolution adaptive optic imaging are poorly efficient. A totally independent technique of binary asteroid discovery, based on astrometry, can help to reveal new binary systems and populate a range of sizes and separations that remain nearly unexplored. In this work, we describe a dedicated period detection method and its results for the data set. This method looks for the presence of a periodic signature in the orbit post-fit residuals. After conservative filtering and validation based on statistical and physical criteria, we are able to present a first sample of astrometric binary candidates, to be confirmed by other observation techniques such as photometric light curves and stellar occultations.

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Deficit of primitive compositions in binary asteroids and pairs

Cited by 6 publications

References 78 publications

Direct N-body Simulations of Satellite Formation around Small Asteroids: Insights from DART’s Encounter with the Didymos System

Direct N-body Simulations of Satellite Formation around Small Asteroids: Insights from DART’s Encounter with the Didymos System

Regolith resurfacing and shedding on spinning spheroidal asteroids: Dependence on the surface mechanical properties

Binary asteroid candidates in Gaia DR3 astrometry

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