TOI-837 b has a true obliquity of 25.9+7.5-6.3 deg, the first planet younger than 100 Myr with accessible ψ incompatible with an aligned orbit, favoring primordial disc torque followed by disc-driven migration.
, year = 1996, month = feb, volume =
12 Pith papers cite this work. Polarity classification is still indexing.
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Bi-CFM learns bidirectional mappings between initial and final state distributions to solve ill-posed inverse problems in chaotic systems, reporting metric improvements and speedups on Lorenz variants plus conservation-respecting results on three-body and globular cluster data.
GW190814 is proposed to originate from a collapsar-disk fragment merging with the central black hole, potentially preceded by SN2019npv ~60 days earlier, yielding H0 = 70.5 (+9.2, -6.4) km/s/Mpc.
N-body simulations show that 14 Herculis's orbital architecture requires primordial ejection of an additional massive planet.
Viscous stirring via gravitational scattering produces lognormal inclination distributions that yield Lorentzian vertical density profiles, which relax to Gaussians after equipartition, enabling estimates of perturber masses in ARKS debris disks.
TOI-1710 b has a true obliquity of 149 degrees indicating retrograde motion, favoring high-eccentricity migration via planet-planet scattering and Kozai-Lidov cycles for this tidally detached super-Neptune.
Archival RV and astrometric data plus three-body simulations constrain an unseen outer perturber in the GJ 436 system to sub-Jovian masses at a_c ≳ 6.8 AU, supporting Kozai-Lidov migration as the source of the hot Neptune's polar eccentric orbit.
Four-planet systems exhibit exponentially increasing lifetimes with orbital spacing, intermediate between three- and five-planet systems, with resonances causing shorter lifetimes and third-order MMRs adding destabilization near certain spacings.
TOI-1533 hosts an inner sub-Neptune (P=3.63 d, R=3.15 R⊕) and outer super-Neptune-mass hot giant (P=8.06 d, R>7.5 R⊕, M≈40 M⊕, ρ<0.48 g cm⁻³) both transiting an active K-dwarf.
Barnard's Star planets have masses 0.19-0.84 M_earth, are tidally locked, unlikely to retain primary atmospheres, and possess mantles rich in ferropericlase with less than half Earth's water capacity and radiogenic heating.
N-body simulations demonstrate long-term dynamical stability of the HD 20794 system across a range of inclinations, with planet d identified as the lowest-mass high-eccentricity HZ-crossing planet.
An upgraded planet population synthesis model incorporates post-disc dynamical evolution and atmospheric enrichment to generate synthetic exoplanet populations with improved fidelity to N-body results and observations.
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Orbital Stability of Closely-Spaced Four-planet Systems
Four-planet systems exhibit exponentially increasing lifetimes with orbital spacing, intermediate between three- and five-planet systems, with resonances causing shorter lifetimes and third-order MMRs adding destabilization near certain spacings.