Rapid escape of ultra-hot exoplanet atmospheres driven by Hydrogen Balmer absorption

TL;DR

This paper reveals a new mechanism for atmospheric escape in ultra-hot exoplanets, driven by stellar near-ultraviolet emission exciting hydrogen, which can lead to rapid mass loss especially around hot stars like KELT-9b.

Contribution

It introduces the concept of Balmer-driven atmospheric escape, highlighting its significance over EUV-driven escape for planets around hot stars, and predicts catastrophic mass loss in certain exoplanets.

Findings

KELT-9b likely exhibits Balmer-driven escape.

Near-ultraviolet emission dominates over EUV in driving escape.

Potential for rapid mass loss in sub-Jupiter mass planets close to hot stars.

Abstract

Atmospheric escape is key to explaining the long-term evolution of planets in our Solar System and beyond, and in the interpretation of atmospheric measurements. Hydrodynamic escape is generally thought to be driven by the flux of extreme ultraviolet photons that the planet receives from its host star. Here, we show that the escape from planets orbiting hot stars proceeds through a different yet complementary process: drawing its energy from the intense near ultraviolet emission of the star that is deposited within an optically thin, high-altitude atmospheric layer of hydrogen excited into the lower state of the Balmer series. The ultra-hot exoplanet KELT-9b likely represents the first known instance of this Balmer-driven escape. In this regime of hydrodynamic escape, the near ultraviolet emission from the star is more important at determining the planet mass loss than the extreme ultraviolet emission, and uncertainties in the latter become less critical. Further, we predict that gas exoplanets around hot stars may experience catastrophic mass loss when they are less massive than 1--2 Jupiter masses and closer-in than KELT-9b, thereby challenging the paradigm that all large exoplanets are stable to atmospheric escape. We argue that extreme escape will affect the demographics of close-in exoplanets orbiting hot stars.