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.
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19 Pith papers cite this work. Polarity classification is still indexing.
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HST/WFC3 UV imaging of SR 12 c measures accretion luminosity of 1.65 ± 0.19 × 10^{-5} L_⊙ and rate of 8 ± 2 × 10^{-12} M_⊙ yr^{-1}, placing it at the end stages of giant planet assembly with a full UV-to-sub-mm SED.
Observations of the HK Tau binary with JWST reveal gas-phase molecular lines in the low-inclination primary and ice absorption features in the edge-on secondary, enabled by their differing inclinations.
Panchromatic JWST spectrum of WASP-121 b detects SiO and measures refractory-to-volatile ratios 3x stellar, consistent with mixed solid-gas accretion or migration with continued solid accretion.
A spectral-multigrid Poisson solver for spherical and cylindrical coordinates achieves second-order accuracy on uniform and logarithmic radial grids with vacuum boundary handling via screening mass and scales to 4096 cores.
N-body simulations find stellar mass-loss effects dominate gravitational scattering in altering giant planet orbits around white dwarfs formed in star clusters, independent of density and initial conditions.
A brown-dwarf companion's close pericenter in KELT-20 imposes dynamical limits that disfavor giant planet formation beyond the water-ice line.
Three accelerating stars yield one stellar companion at 166 AU, one 45 Jupiter-mass object at ~18 AU, and one 9.5 Jupiter-mass object at 6.4 AU that is 65% likely to be a planet.
TOI-5882, a lithium-enriched subgiant with a brown dwarf companion, shows enrichment consistent with engulfment of a super-Earth to Neptune-mass planet.
Atmospheric retrievals on CRIRES+ spectra of 2MASS J0249-0557 c and two eta Pic YMG brown dwarfs give solar-like C/O, metallicity, and carbon isotope ratios, supporting gravitational collapse formation for the companion.
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.
Reanalysis of 79 solar twins indicates the Sun's chemical peculiarity is largely explained by Galactic chemical evolution, with 2-6 candidates possibly showing planetary engulfment.
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.
Retrievals on six isolated brown dwarfs yield near-solar C/O (0.51-0.63), metallicities, and 12C/13C ratios (91-155) supporting molecular cloud fragmentation origin.
H-type objects in IC348 show spatial distributions matching stars and brown dwarfs, unlike the more dispersed distribution of simulated ejected planets, indicating a star-like formation origin.
Three new hot Jupiters (periods 1.8-4 days, radii 1.22-1.58 RJup, masses 0.36-0.87 MJup) around evolved stars aged 4-9 Gyr, extending the sample for hot Jupiter evolutionary studies.
TOI-7154b is a 71.7 M_J brown dwarf in an 8.86-day eccentric orbit around a G star, with eccentricity and age suggesting stellar-like fragmentation origins.
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.
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
citing papers explorer
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Ultraviolet Imaging of SR 12 c with HST/WFC3: Accretion and Variability of a Giant Planet at the End Stages of Growth
HST/WFC3 UV imaging of SR 12 c measures accretion luminosity of 1.65 ± 0.19 × 10^{-5} L_⊙ and rate of 8 ± 2 × 10^{-12} M_⊙ yr^{-1}, placing it at the end stages of giant planet assembly with a full UV-to-sub-mm SED.