A chemical kinetics code for modelling exoplanetary atmospheres. Issue 2 (16th May 2019)

• Record Type: Journal Article
• Authors: Hobbs, Richard; Shorttle, Oliver; Madhusudhan, Nikku; Rimmer, Paul
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 487:Issue 2(2019)
• Page Start: 2242
• Page End: 2261
• Publication Date: 2019-05-16
• Subjects: planets and satellites: atmospheres -- planets and satellites: composition -- planets and satellites: gaseous planets -- planets and satellites: individual (HD 189733b, HD 209458b); Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz1333
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: Chemical compositions of exoplanets can provide key insights into their physical processes and formation and evolutionary histories. Atmospheric spectroscopy provides a direct avenue to probe exoplanetary compositions. However, whether obtained in transit or thermal emission, spectroscopic observations probe limited pressure windows of planetary atmospheres and are directly sensitive to only a limited set of spectroscopically active species. It is therefore critical to have chemical models that can relate retrieved atmospheric compositions to an atmosphere's bulk physical and chemical state. To this end, we present Levi a new chemical kinetics code for modelling exoplanetary atmospheres. Levi calculates the gas phase hydrogen, oxygen, carbon, and nitrogen chemistry in planetary atmospheres. Here, we focus on hot gas giants. Applying Levi, we investigate how variations in bulk C/O and N/O affects the observable atmospheric chemistry in hot Jupiters. For typical hot Jupiters, we demonstrate the strong sensitivity of molecular detections to the atmospheric C/O. Molecular detections are conversely less sensitive to the atmospheric N/O ratio, although highly supersolar N/O can decrease the C/O required for HCN and NH3 detection. Using a new pressure–temperature (P–T) profile for HD 209458b without a thermal inversion, we evaluate recently reported detection's of CO, H2 O, and HCN in its day-side atmosphere. We find that our models are consistent with the detected species, albeit with a narrow compositional window around C/O ∼ 1. A C/O ≳ 0.9 (1.6 times solar) was required to meet the minimum reported value for HCN, while a C/O ≲ 1 (1.8 times solar) was required to fit the nominal H2 O abundance.