Detection of Yarkovsky acceleration in the context of precovery observations and the future<i>Gaia</i>catalogue

Desmars, J.

doi:10.1051/0004-6361/201423685

Cited by 15 publications

(11 citation statements)

References 27 publications

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“…The typical value of the Yarkovsky acceleration for a subkilometer NEA is 10 −15 -10 −13 au/day 2 (Del Vigna et al 2018). Though small, the Yarkovsky effect may influence the long-term orbital evolution of asteroids (Desmars 2015). Two teams of investigators have comprehensively studied the short-and long-term dynamics of HO3: De la Fuente Marcos & De la Fuente Marcos (2016) and .…”

Section: Introductionmentioning

confidence: 99%

“…Vokrouhlický et al (2008) detected the Yarkovsky-related drift using only ground-based astrometric observations of the asteroid (152563) 1992BF. Subsequently, the Yarkovsky-related drifts of a large number of NEAs were detected using ground-based optical astrometry (Del Vigna et al 2018;Desmars 2015;Farnocchia et al 2013;Greenberg et al 2020;Nugent et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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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%

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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“…While it seems nearly certain that numerous detections of the Yarkovsky effect will emerge from current and upcoming astrometric surveys in the next decade (e.g., Delbò et al, 2008;Mouret and Mignard, 2011;Nugent et al, 2012b;Desmars, 2015), more work is needed to secure YORP detections, especially across the whole range of possible rotation periods. This should help us understand in what proportion the YORP effect results in acceleration or deceleration of the rotation rate.…”

Section: Discussionmentioning

confidence: 99%

The Yarkovsky and YORP Effects

Vokrouhlicky,

Bottke,

Chesley

et al. 2015

Preprint

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The Yarkovsky effect describes a small but significant force that affects the orbital motion of meteoroids and asteroids smaller than 30 − 40 kilometers in diameter. It is caused by sunlight; when these bodies heat up in the Sun, they eventually re-radiate the energy away in the thermal waveband, which in turn creates a tiny thrust. This recoil acceleration is much weaker than solar and planetary gravitational forces, but it can produce measurable orbital changes over decades and substantial orbital effects over millions to billions of years. The same physical phenomenon also creates a thermal torque that, complemented by a torque produced by scattered sunlight, can modify the rotation rates and obliquities of small bodies as well. This rotational variant has been coined the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. During the past decade or so, the Yarkovsky and YORP effects have been used to explore and potentially resolve a number of unsolved mysteries in planetary science dealing with small bodies. Here we review the main results to date, and preview the goals for future work.

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“…This event was one of a number aimed at characterizing the sizes, shapes and surroundings of TNO's and Centaurs (Assafin et al, 2012;Camargo et al, 2014), and monitoring Pluto's atmosphere (Assafin et al, 2010). In the case of Chariklo, a further incentive was the search for surrounding (possibly cometary) material, as both sharp and diffuse secondary events were detected in 1993 and 1994 Desmars (2015); Desmars et al (2015). b Fornasier et al (2014).…”

Section: The Discovery Of Chariklo's Ringsmentioning

confidence: 99%