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From the 1 of 6 linked papers with an AI index.

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6 papers

astro-ph.EP2026

The SPACE Program II: No discernible spectral features in the transmission spectrum of the sub-Neptune HD 191939 b observed with HST/WFC3

Cyril Gapp, Lorena Acuña-Aguirre, Reza Ashtari +17

The atmospheres of sub-Neptunes provide a window into their internal structure and history, shedding light on the origin of this common, but enigmatic, class of exoplanets. However…

astro-ph.EP2026

The majority of hot Jupiters formed beyond the water ice line

Yaxing He, Bertram Bitsch, Adrien Houge +2

The paper uses planet formation simulations to show that the atmospheric compositions of hot Jupiters suggest most of them formed beyond the water ice line and later migrated inwar…

astro-ph.EP2026

The panchromatic JWST dayside spectrum of WASP-121 b reveals a refractory-rich formation

K. Angelique Kahle, Paul Mollière, Laura Kreidberg +16

One path to understand how planets form is to link their present-day atmospheric composition to predictions from planet formation models. For the hottest planets, the abundances of…

astro-ph.EP2026

Simulating the interplay between the snowline pebble flux and ongoing planet formation and migration

Danila Astrakhantsev, Sebastiaan Krijt, Sofia Savvidou +1

Pebble drift plays a central role in modern planet formation models. In this work we carry out planet formation simulations (including pebble accretion and migration) for a range o…

astro-ph.EP2025

Locked In Ice: how Pebble Drift and Volatile Entrapment can Significantly Impact Carbon and Oxygen Ratios in Evolving Protoplanetary Discs

Joe Williams, Sebastiaan Krijt, Bertram Bitsch +2

The complex interplay between the growth, drift, and sublimation of ice-covered pebbles can strongly influence the volatile distribution and evolution of disc composition, and ther…

astro-ph.EP2025

Aligned Stellar Obliquities for Two Hot Jupiter-hosting M Dwarfs Revealed by MAROON-X: Implications for Hot Jupiter Formation

Drew Weisserman, Erik Gillis, Ryan Cloutier +14

Hot Jupiters (HJs) are less common around early M dwarfs than around AFGK stars, suggesting that HJs may form and/or migrate via distinct pathways around different type…