Reviews

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.

Contains a list of specific asteroids that are in secular resonances. Useful for comparison or software testing.

Complete list of secular resonances by order with unified notation

A comprehensive overview of existing secular resonances and their classification by dynamic zones. An excellent start for understanding!

Interesting to isolate encounters vs. secular/MMR resonance effects.

Interesting for learning about close encounters and impacts of V-type asteroids with terrestrial planets, but a bit niche.

A dynamical steady-state model links NEO orbits to asteroid-belt resonances, highlighting Yarkovsky drift as the key resupply mechanism. A bit outdated.

Interesting paper to learn about the dynamics of mmr with Venus in the CR3BP model. Advanced, require some background in celestial mechanics.

Useful to learn about what mmr with Earth may be relevant for NEOs. Quite advanced, not an easy reading.