Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry

Mottola, S.; Hellmich, S.; Zangari, A. M.; Stephens, Robert D.; Martino, M. Di; Proffe, Gerrit; Marchi, S.; Olkin, C. B.; Levison, Harold F.

doi:10.3847/psj/acaf79

Cited by 7 publications

(1 citation statement)

References 53 publications

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“…Data in Grav et al (2011) and Grav et al (2012) indicate the albedo distribution for the Trojans becomes much wider below ;30 km (approximately magnitude 11 for albedo value 0.07), but there is no statistically substantial difference between the L4 and L5 populations at these smaller sizes. Additionally, recent observations focused on Lucy mission targets (e.g., Buie et al 2018Buie et al , 2021Mottola et al 2023) found that WISE albedo determinations for Trojans could be systematically too high (an issue possibly related to the shape uncertainty).…”

Section: Bias-corrected L4/l5 Populationsmentioning

confidence: 99%

Orbital and Absolute Magnitude Distribution of Jupiter Trojans

Vokrouhlický,

Nesvorný,

Brož

et al. 2024

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Jupiter Trojans (JTs) librate about the Lagrangian stationary centers L4 and L5 associated with this planet on typically small-eccentricity and moderate-inclination heliocentric orbits. The physical and orbital properties of JTs provide important clues about the dynamical evolution of the giant planets in the early solar system, as well as populations of planetesimals in their source regions. Here we use decade-long observations from the Catalina Sky Survey (station G96) to determine the bias-corrected orbital and magnitude distributions of JTs. We distinguish the background JT population, filling smoothly the long-term stable orbital zone about L4 and L5 points and collisional families. We find that the cumulative magnitude distribution of JTs (the background population in our case) has a steep slope for H ≤ 9, followed by a moderately shallow slope until H ≃ 14.5, beyond which the distribution becomes even shallower. At H = 15 we find a local power-law exponent 0.38 ± 0.01. We confirm the asymmetry between the magnitude-limited background populations in L4 and L5 clouds characterized by a ratio 1.45 ± 0.05 for H < 15. Our analysis suggests an asymmetry in the inclination distribution of JTs, with the L4 population being tighter and the L5 population being broader. We also provide a new catalog of the synthetic proper elements for JTs with an updated identification of statistically robust families (9 at L4, and 4 at L5). The previously known Ennomos family is found to consist of two overlapping Deiphobus and Ennomos families.

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Section: Bias-corrected L4/l5 Populationsmentioning

confidence: 99%

Orbital and Absolute Magnitude Distribution of Jupiter Trojans

Vokrouhlický,

Nesvorný,

Brož

et al. 2024

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Surface Geology of Jupiter’s Trojan Asteroids

Marchi

Bell

Bierhaus³

et al. 2023

Space Sci Rev

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The surface geology of Jupiter’s Trojan asteroids is one of the scientific investigations of the NASA Lucy mission. A dedicated Geology Working Group will implement these studies using primarily panchromatic and color imaging data and complement the interpretation of these data with theoretical models, such as collisional evolution models. The Lucy Science Team will also rely on experience and lessons learned from prior space missions, such as NASA’s NEAR, Dawn, OSIRIS-REx, and New Horizons.A chief goal of the Geology Working Group is to map craters and characterize their morphology across Lucy target’s surfaces over a range of spatial resolutions. These data will be used to constrain the relative and absolute ages of terrains and their impactor size-frequency distributions. More broadly, impact-related processes such as excavation and mass wasting will inform other investigations, including geological unit mapping, stratigraphy and topography, surface composition, and internal structure. Lucy’s cratering data and morphology will also be used to perform comparative analyses with similar data from other small bodies across the Solar System, from Main Belt asteroids to Kuiper Belt objects. The present article provides an overview of the planned activities and methodologies of the Geology Working Group.

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Shapes, Rotations, Photometric and Internal Properties of Jupiter Trojans

Mottola,

Britt,

Brown

et al. 2024

Space Sci Rev

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The Jupiter Trojans, being trapped around the stable L4 and L5 Jupiter Lagrangian points, are thought to be more primitive than the Main Belt asteroids. They are believed to have originated from a range of heliocentric distances in the trans-Neptunian region, to have subsequently been scattered inwards, and finally captured in their current location during the phase of Giant Planet migration. As a consequence, their bulk composition is expected to reflect that of the protoplanetary disk at the time and location of their formation. The photometric properties of Trojans appear to have a bi-modal distribution. A few Trojans have been discovered to be binary systems, suspected contact binaries, or to possess moonlets, which has revealed consistently low bulk densities (around $1\times 10^{3}$ 1 × 10 3 kg $\mathrm {m}^{-3}$ m − 3 ) for those systems. Those estimates, together with the presence of a spin barrier between 4 and 4.8 h rotation period, suggest that low densities are a general property of the population, similar to that of cometary nuclei.Current Trojan physical properties provide clues that relate to their formation that can, in turn, be traced back to the origin of the solar system. We review here our current knowledge on the physical properties of Trojans and the methods used for their determinations. Most of these methods are based on Earth-bound observations, and are limited by the large distance to these objects. The next breakthrough will be made possible by the Lucy mission, which, by visiting several Trojans during a tour through both clouds, will address many open questions and probably raise new ones. The combination of the ground truth for select objects provided by Lucy with the context view given by the Earth-bound observations will result in powerful synergy.

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Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry

Cited by 7 publications

References 53 publications

Orbital and Absolute Magnitude Distribution of Jupiter Trojans

Orbital and Absolute Magnitude Distribution of Jupiter Trojans

Surface Geology of Jupiter’s Trojan Asteroids

Shapes, Rotations, Photometric and Internal Properties of Jupiter Trojans

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