Hydrogen escaping from a pair of exoplanets smaller than Neptune
Schreyer, Ethan; Owen, James E.; Loyd, R. O. Parke; Murray-Clay, Ruth; Peacock, Sarah; Batalha, Natasha E.; Barman, Travis; France, Kevin; Youngblood, Allison; Ardila, David R.; Teske, Johanna; Shkolnik, Evgenya L.; Schneider, Adam C.; Giacalone, Steven; Schneider, P. Christian; Duvvuri, Girish M.; Schlichting, Hilke E.; Wilson, David J.; Rogers, James G.; Longo, Isabella; Broome, Madelyn I.
United States, United Kingdom, Germany
Abstract
Exoplanet surveys have shown a class of abundant exoplanets smaller than Neptune on close, <100-day orbits1, 2, 3–4. These planets form two populations separated by a natural division at about 1.8 R⊕ termed the radius valley. It is uncertain whether these populations arose from separate dry versus water-rich formation channels, evolved apart because of long-term atmospheric loss or a combination of both5, 6, 7, 8, 9, 10, 11, 12, 13–14. Here we report observations of ongoing hydrogen loss from two sibling planets, TOI-776 b (1.85 ± 0.13 R⊕) and TOI-776 c (2.02 ± 0.14 R⊕), the sizes of which near the radius valley and mature (1–4 Gyr) age make them valuable for investigating the origins of the divided population of which they are a part. During the transits of these planets, absorption appeared against the Lyman-α emission of the host star, compatible with hydrogen escape at rates equivalent to 0.03–0.6% and 0.1–0.9% of the total mass per billion years of each planet, respectively. Observations of the outer planet, TOI-776 c, are incompatible with an outflow of dissociated steam, suggesting both it and its inner sibling formed in a dry environment. These observations support the strong role of hydrogen loss in the evolution of close-orbiting sub-Neptunes5, 6, 7–8,15,16.