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Lunar crater identification via deep learning

arXiv (opens in a new tab)

A STATISTICAL RECONSTRUCTION OF THE PLANET POPULATION AROUND KEPLER SOLAR-TYPE STARS

Using the cumulative catalog of planets detected by the NASA Kepler mission, we reconstruct the intrinsic occurrence of Earth- to Neptune-size (1–4 R⊕) planets and their distributions with radius and…
IOP Publishing (opens in a new tab)

Hybrid symplectic integrators for planetary dynamics

Hybrid symplectic integrators such as MERCURY are widely used to simulate complex dynamical phenomena in planetary dynamics that could otherwise not be investigated. A hybrid integrator achieves…
arXiv (opens in a new tab)

Predicting the long-term stability of compact multiplanet systems

The Stability of Planetary Orbital Configurations Klassifier (SPOCK) predicts stability using physically motivated summary statistics measured in integrations of the first 104 orbits, thus achieving speed-ups of up to 105 over full simulations, which computationally opens up the stability-constrained characterization of multiplanet systems.
NAS (opens in a new tab)

A MACHINE LEARNS TO PREDICT THE STABILITY OF TIGHTLY PACKED PLANETARY SYSTEMS

It is found that training an XGBoost machine-learning algorithm on physically motivated features yields an accurate classifier of stability in packed systems, and motivates investing computational resources to train algorithms capable of predicting stability over longer timescales and over broader regions of phase space.
IOP Publishing (opens in a new tab)

Tides alone cannot explain Kepler planets close to 2:1 MMR

A number of Kepler planet pairs lie just wide of first-order mean motion resonances (MMRs). Tides have been frequently proposed to explain these pileups, but it is still an ongoing discussion. We…
arXiv (opens in a new tab)

Machine Learning Algorithms For Predicting the Instability Timescales of Compact Planetary Systems

Predicting Instability Timescales in Closely-Packed Planetary Systems

Tidal Forces Cannot Explain Planets Close to 2:1 Mean Motion Resonance

Statistics, Formation and Stability of Exoplanetary Systems

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