Roche lobe overflow during gas giant destruction aligns stellar spins with orbits within tens of degrees regardless of starting conditions, offering an observable to differentiate this mechanism from high-eccentricity migration.
Title resolution pending
8 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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astro-ph.EP 8years
2026 8verdicts
UNVERDICTED 8representative citing papers
Roche lobe overflow destruction of hot Jupiters clears all companions from the sub-Jovian desert inside ~4 days while most observed companions remain stable, unlike tidal disruption during high-eccentricity migration.
Wind speed measurements in seven ultra-hot Jupiters decrease with temperature, consistent with magnetic drag and implying magnetic field strengths of a few gauss.
Dynamical tides exciting f-modes during high-eccentricity migration produce the hot Jupiter pile-up, Neptune ridge, and Neptune desert via orbital circularization and selective atmospheric mass loss.
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.
Hydrogen-silicate miscibility stores hydrogen in sub-Neptune interiors, resupplies escaping envelopes, delays contraction, matches young-planet observations, and enables a population test requiring 70-100 targets under 100 Myr.
Reanalysis of TOI-1272 and TOI-1694 retracts TOI-1272 c as planetary, attributes the signal to stellar activity via Gaussian process modeling, and refines orbital parameters for the systems.
Detection and characterization of two eccentric warm Jupiters TOI-2147 b (P=26.2 d, e=0.29, M=116 M⊕) and TOI-6019 b (P=14.5 d, e=0.48, M=149 M⊕) with TESS and MaHPS data, showing mildly inflated radii consistent with tidal heating.
citing papers explorer
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Revealing the Origin of Desert Dwellers via Stellar Obliquities
Roche lobe overflow during gas giant destruction aligns stellar spins with orbits within tens of degrees regardless of starting conditions, offering an observable to differentiate this mechanism from high-eccentricity migration.
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Stability of Multiplanet Systems Through Hot Jupiter Destruction
Roche lobe overflow destruction of hot Jupiters clears all companions from the sub-Jovian desert inside ~4 days while most observed companions remain stable, unlike tidal disruption during high-eccentricity migration.
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Magnetic field strengths of hot giant exoplanets consistent with Solar System values
Wind speed measurements in seven ultra-hot Jupiters decrease with temperature, consistent with magnetic drag and implying magnetic field strengths of a few gauss.
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Dynamical Tides during High-Eccentricity Migration produces the Hot Jupiter Pile-up, Neptune Ridge, and Neptune Desert
Dynamical tides exciting f-modes during high-eccentricity migration produce the hot Jupiter pile-up, Neptune ridge, and Neptune desert via orbital circularization and selective atmospheric mass loss.
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A tidally detached super Neptune on a strongly misaligned retrograde orbit
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.
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Testing the prevalence of hydrogen-silicate miscibility in young sub-Neptunes
Hydrogen-silicate miscibility stores hydrogen in sub-Neptune interiors, resupplies escaping envelopes, delays contraction, matches young-planet observations, and enables a population test requiring 70-100 targets under 100 Myr.
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The GAPS Programme at TNG LXXIV. A reanalysis of the planetary systems TOI-1272 and TOI-1694 with HARPS-N and retraction of the planetary interpretation of TOI-1272 c
Reanalysis of TOI-1272 and TOI-1694 retracts TOI-1272 c as planetary, attributes the signal to stellar activity via Gaussian process modeling, and refines orbital parameters for the systems.
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TOI-2147 b and TOI-6019 b: Two eccentric warm Jupiters detected and characterized with TESS and MaHPS
Detection and characterization of two eccentric warm Jupiters TOI-2147 b (P=26.2 d, e=0.29, M=116 M⊕) and TOI-6019 b (P=14.5 d, e=0.48, M=149 M⊕) with TESS and MaHPS data, showing mildly inflated radii consistent with tidal heating.