Five carbon- and nitrogen-bearing species in a hot giant planet's atmosphere

TL;DR

This study detects multiple carbon- and nitrogen-bearing molecules in the atmosphere of hot Jupiter HD 209458b, revealing a carbon-rich composition that challenges the common assumption of solar-like, oxygen-rich atmospheres in such exoplanets.

Contribution

It provides the first comprehensive detection of several molecules in HD 209458b's atmosphere, indicating a carbon-rich chemistry and suggesting a different planet formation and migration history.

Findings

Detection of H2O, CO, HCN, CH4, NH3, and C2H2 with high statistical significance.

Evidence for a carbon-to-oxygen ratio near or above 1, higher than solar.

Implication of formation far from the current orbit and inward migration.

Abstract

The atmospheres of gaseous giant exoplanets orbiting close to their parent stars (hot Jupiters) have been probed for nearly two decades. They allow us to investigate the chemical and physical properties of planetary atmospheres under extreme irradiation conditions. Previous observations of hot Jupiters as they transit in front of their host stars have revealed the frequent presence of water vapour and carbon monoxide in their atmospheres; this has been studied in terms of scaled solar composition under the usual assumption of chemical equilibrium. Both molecules as well as hydrogen cyanide were found in the atmosphere of HD 209458b, a well studied hot Jupiter (with equilibrium temperature around 1,500 kelvin), whereas ammonia was tentatively detected there and subsequently refuted. Here we report observations of HD 209458b that indicate the presence of water (H2O), carbon monoxide (CO), hydrogen cyanide (HCN), methane (CH4), ammonia (NH3) and acetylene (C2H2), with statistical significance of 5.3 to 9.9 standard deviations per molecule. Atmospheric models in radiative and chemical equilibrium that account for the detected species indicate a carbon-rich chemistry with a carbon-to-oxygen ratio close to or greater than 1, higher than the solar value (0.55). According to existing models relating the atmospheric chemistry to planet formation and migration scenarios, this would suggest that HD 209458b formed far from its present location and subsequently migrated inwards. Other hot Jupiters may also show a richer chemistry than has been previously found, which would bring into question the frequently made assumption that they have solar-like and oxygen-rich compositions.