Reviews

By developing and numerically verifying an analytical model that includes Yarkovsky–Schach and planetary thermal effects, the researchers demonstrated that the Yarkovsky force significantly impacts mutual binary orbits. This orbital evolution occurs specifically in non-synchronous systems, where the spin and orbital periods differ, opening up new possibilities for understanding how binary systems migrate over time.

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This study provides comprehensive data on Yarkovsky-driven changes in eccentricity and longitude of periapse. By exploring a broad range of physical and orbital parameters, the results complement the drift rates in semi-major axis previously established by Spitale and Greenberg (2001).

It is shown that the average thermal inertia of a sample of NEAs in the km-size range is 200 ± 40 J m^−2 s^−0.5 K^−1 and it is identified a trend of increasing thermal inertia with decreasing asteroid diameter.

Arecibo radar ranging of NEA 6489 Golevka (diameter ~ 0.5 km) confirms the presence of Yarkovsky-driven orbital drift. This non-gravitational perturbation was isolated by comparing the asteroid's observed trajectory against purely Newtonian dynamical models.

By developing and numerically verifying an analytical model that includes Yarkovsky–Schach and planetary thermal effects, the researchers demonstrated that the Yarkovsky force significantly impacts mutual binary orbits. This orbital evolution occurs specifically in non-synchronous systems, where the spin and orbital periods differ, opening up new possibilities for understanding how binary systems migrate over time.

By measuring non-gravitational orbital drift, this study identifies the Yarkovsky effect across the NEA population. The reliability of these detections is maintained through a high-precision model—incorporating relativistic terms and the mass of 16 large asteroids—combined with specialized astrometric error treatment.

They used the determined rotation state, shape, size and thermophysical model of Apophis to predict the strength of the Yarkovsky effect in its orbit.

In this paper was investigated the possibility of detecting the Yarkovsky effect via precise orbit determination of near-Earth asteroids.

The study summarizes the knowledge about Yarkovsky, YORP, BYORP effects up to 2015.

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The purpose of this paper is to draw attention to failures in computation of asteroid synthetic proper elements with a goal to point out the dynamical or computational causes of the failures.

They computed Lyapunov times for a sample of trans-Neptunian objects and outer main-belt asteroids using three numerical approaches: the variational method and two implementations of the renormalization technique.

It is presented an analysis of the reliability of computation of maximum Characteristic Exponents of Lyapunov from the numerical integrations of asteroid orbits over finite intervals of time.

It is presented a simple approach to estimating the contribution of the radial component of the LCE to identify trajectories in the “confined chaos” regime.

It is studied the dynamical orbital and physical evolution of all 21 numbered and 13 selected unnumbered asteroids in retrograde orbits. They computed their starting orbital elements, absolute magnitudes, and diameters, together with the non-gravitational parameters A2 and da/dt.

It is showed that many three-body resonances involving the longitude of Saturn are chaotic. They gave simple expressions for the width of the chaotic region and the associated Lyapunov time.

Their findings suggest that for relatively spheroidal bodies composed of small-scale debris, such as Dimorphos, the BYORP effect may be significantly weaker and more sensitive to the object's size than earlier models predicted.

While the origin of similar binaries (primary and satellite) in these two dynamically different populations (MB and NEA) was previously unknown, here is showed that they form via YORP-induced spin-up of 'rubble pile' asteroids.

They demonstrate that the Near-Earth Asteroids 2017 SN16 and 2018 RY7 currently follow an orbital path where their relative mean longitude remains stable. This lack of long-term drift is a direct result of the stabilizing influence of the 3:5 MMR with Venus.

Authors derived and estimated many astrometric and physical parameters about 93 genetically connected asteroid pairs.

This research examines how strong the material of 'contact binary' asteroids must be to allow them to fuse into a single object.

This study explores the detection of binary systems via the astrometric shift of the photocenter relative to the barycenter. By utilizing this "wobble," we can probe regions of the binary asteroid phase-space that remain challenging for standard observational techniques to reach.