Reviews

An excellent overview article on self-determination theory. A bit shorter than the book. Useful for a “quick” understanding of the theory.

An empirical measure within the framework of Self-Determination Theory that identifies causal orientation (autonomous, external, or impersonal). The primary instrument for the corresponding construct.

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.

Observational data confirms that binaries smaller than 20 km typically originate from rotational fission, a process driven by the YORP effect. This suggests a comprehensive framework where rotational fission and subsequent dynamical evolution account for the creation of small-scale binary, triple, and paired asteroid systems.

This study details a specialized period-detection algorithm and presents its application to the Gaia DR3 catalog. The technique identifies periodic signatures by analyzing the post-fit residuals of the calculated orbits.

Here are devised two equations that approximately describe the functional relation between the average time dtr spent in the three-body resonance, the strength of the resonance SR, and the semimajor axis drift speed da/dt (positive and negative) with the orbital eccentricities of asteroids in the range (0, 0.1).

Here is derived a functional relation that accurately describes dependence between the average time lead/lag dtr in mean motion resonances, the strength of the resonance SR, and the semimajor axis drift speed da/dt with asteroids’ orbital eccentricities in the range (0.1, 0.2).

The main conclusion of this study is: the location of the inverse of the ‘limiting’ diameter 1/D(limit) (derived from the ‘limiting’ Yarkovsky drift speed, 7 × 10^(−5) au/Myr) is exactly at the place of changing the V-shape slope of the border in an old asteroid family which are crossed in the same side by relatively strong mean motion resonance, very close to the parent body, in the (a, 1/D) plane.

This paper has presented a new description on the orbital behavior of resonant asteroids with very small Yarkovsky drift speeds. The conclusion is the boundary value of da/dt in the motion of resonant main belt asteroids under the influence of the Yarkovsky effect is at |−7| ×10^(−5) au/Myr. Below this value, asteroids typically quickly jump across the mean motion resonances, and this is especially the case in strong resonances, such as 9:4, 8:3 and 13:6 with Jupiter.

It would be easy to calculate the average time that an object spent inside an mean-motion resonance, with given the resonance’s strength, the Yarkovsky drift speed and an object’s eccentricity (0.025<e<0.4). The derived modified Laplace statistical distribution could be used for generating the average time for certain number of asteroids with a particular Yarkovsky drift speed in mean motion resonances.

This Letter presents a novel view on the interaction between mean-notion resonances and the Yarkovsky effect, describing for the first time the functional relationship between the average time spent inside a resonance, the strength of the resonance, and the semimajor axis drift speed.

If you need to identify whether or not an asteroid is trapped in secular resonance, this is the package for you.