Near-Earth Asteroid Characterization and Observation (NEACO) Mission to Asteroid (469219) 2016 HO3

Venigalla, Chandrakanth; Baresi, Nicola; Aziz, Jonathan; Bercovici, Benjamin; Brack, D. N.; Dahir, Andrew; Smet, Sarah De; Fulton, JoAnna; Pellegrino, Marielle M.; wal, S. Van

doi:10.2514/1.a34268

Cited by 23 publications

(7 citation statements)

References 29 publications

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“…HO3 is a perfect example of such a quasi-satellite and is also currently the closest to Earth, being always between 38 and 100 times the distance of the Moon (The Earth's Hill sphere is about four times the Earth-Moon distance). Therefore, several space-exploration missions to the asteroid HO3 have been proposed (Wiegmann 2018;Heiligers et al 2019;Venigalla et al 2019;CNSA 2019). Among these is the future Chinese Tianwen-2 small body exploration mission, which is a sample-return visit to HO3 planned for sometime around 2024 (CNSA 2019;Jin et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Yarkovsky effect detection from ground-based astrometric data for near-Earth asteroid (469219) Kamo’oalewa

Liu

Yan

et al. 2022

A&A

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Context. The Yarkovsky effect is a weak non-gravitational force but may significantly affect subkilometer-sized near-Earth asteroids. Yarkovsky-related drift may be detected, in principle, from astrometric or radar datasets of sufficient duration. To date, the asteroid Kamo'oalewa, the most stable of Earth's quasi-satellites, has an ∼ 18 year-long arc of ground-based optical astrometry. These data provide an opportunity to detect the Yarkovsky effect acting on the asteroid Kamo'oalewa. Aims. We determined the Yarkovsky-related drift of asteroid Kamo'oalewa from ∼ 18 years of ground-based optical astrometry. Furthermore, we investigated the influence of the Yarkovsky effect on the orbital evolution of asteroid Kamo'oalewa based on this estimated value, and evaluated the potential improvements in the detection of non-gravitational accelerations (Yarkovsky effect and solar radiation pressure) for the asteroid Kamo'oalewa that could be provided by the future Chinese small-body exploration mission, Tianwen-2. Methods. The Yarkovsky-related drift of asteroid Kamo'oalewa was detected from the orbital fitting of the astrometry measurements. We checked the Yarkovsky effect detection based on both the orbit fitting results and the physical mechanisms of the Yarkovsky effect. Results. We report for the first time the detection of the Yarkovsky effect acting on asteroid Kamo'oalewa based on ∼ 18 years of ground-based optical astrometry data. The estimated semi-major axis drift is (-6.155 ± 1.758) × 10 −3 au/Myr. In addition, our numerical simulation shows that the Yarkovsky effect has almost no influence on the short-term orbital evolution of the asteroid Kamo'oalewa, but does have a long-term influence, by delaying the entry of the object into the Earth co-orbital region and accelerating its exit from this region, with a more significant signature on the exit than on the entry. In the context of spacecraft tracking data, the Tianwen-2 mission will improve both non-gravitational accelerations (Yarkovsky effect and solar radiation pressure) and predictions of its future ephemeris.

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Section: Introductionmentioning

confidence: 99%

Yarkovsky effect detection from ground-based astrometric data for near-Earth asteroid (469219) Kamo’oalewa

Liu

Yan

et al. 2022

A&A

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“…We consider the NEO (469219) Kamo'oalewa, which is in 1:1 mean motion resonance with the Earth. The astronomical community gave a lot of attention to this object upon its discovery, because it is currently in a quasi-satellite configuration with the Earth, meaning that the critical angle σ librates around zero, and therefore it is easily accessible for space missions (Venigalla et al, 2019). Completely numerical studies of both the short (de la Fuente Marcos and de la Fuente Marcos, 2016) and the long-term dynamics (Fenucci and Novaković, 2021) have been performed.…”

Section: Case B2mentioning

confidence: 99%

Proper elements for resonant planet-crossing asteroids

Fenucci,

Gronchi,

Saillenfest

2022

Preprint

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Proper elements are quasi-integrals of motion, meaning that they can be considered constant over a certain timespan, and they permit to describe the long-term evolution with a few parameters. Near-Earth objects (NEOs) generally have a large eccentricity and therefore they can cross the orbits of the planets. Moreover, some of them are known to be currently in a mean-motion resonance with a planet. Thus, the methods previously used for the computation of main-belt asteroid proper elements are not appropriate for such objects.In this paper, we introduce a technique for the computation of proper elements of planetcrossing asteroids that are in a mean motion resonance with a planet. First, we numerically average the Hamiltonian over the fast angles while keeping all the resonant terms, and we describe how to continue a solution beyond orbit crossing singularities. Proper elements are then extracted from a frequency analysis of the averaged orbit-crossing solutions. We give proper elements of some known resonant NEOs, and provide comparisons with nonresonant models. These examples show that it is necessary to take into account the effect of the resonance for the computation of accurate proper elements.

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“…This can be contrasted with Earth's first-known recurrent quasi-satellite, asteroid 2002 AA 29 , whose future predicted QS state will last only for a few decades [12,13]. Kamo'oalewa's close proximity to Earth and its unknown dynamical origin make it a scientifically compelling candidate for a future space mission [14,15].…”

Section: Introductionmentioning

confidence: 99%

Orbital pathways for a Lunar-Ejecta Origin of the Near-Earth Asteroid Kamo`oalewa

Malhotra

Rosengren²,

Castro-Cisneros

2023

Preprint

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The near-Earth asteroid, Kamo‘oalewa (469219), is one of a small number of known quasi-satellites of Earth. Numerical simulations show that it transitions between quasi-satellite and horseshoe orbital states on centennial timescales, maintaining this dynamics over megayears. Its reflectance spectrum suggest a similarity to lunar silicates. Considering its Earth-like orbit and its physical resemblance to lunar surface materials, we explore the hypothesis that it might have originated as a debris-fragment from a meteoroidal impact with the lunar surface. We carry out numerical simulations of the dynamical evolution of particles launched from different locations on the lunar surface with a range of ejection velocities. As these ejecta escape the Earth-Moon environment and evolve into heliocentric orbits, we find that a small fraction of launch conditions yield outcomes that are compatible with Kamo‘oalewa’s dynamical behavior. The most favored conditions are launch velocities slightly above the escape velocity from the trailing lunar hemisphere.

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Near-Earth Asteroid Characterization and Observation (NEACO) Mission to Asteroid (469219) 2016 HO3

Cited by 23 publications

References 29 publications

Yarkovsky effect detection from ground-based astrometric data for near-Earth asteroid (469219) Kamo’oalewa

Yarkovsky effect detection from ground-based astrometric data for near-Earth asteroid (469219) Kamo’oalewa

Proper elements for resonant planet-crossing asteroids

Orbital pathways for a Lunar-Ejecta Origin of the Near-Earth Asteroid Kamo`oalewa

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