On the volatile enrichments and heavy element content in HD 189733b

TL;DR

This paper models the volatile and heavy element content of HD 189733b, reconciling spectroscopic data with internal structure models, and suggests the presence of complex carbon molecules in its atmosphere.

Contribution

It introduces a formation and composition model for HD 189733b's envelope that aligns spectroscopic and structural data, highlighting the role of carbon molecules.

Findings

Range of volatile abundances consistent with heavy element estimates

Supersolar carbon and oxygen abundances fit spectral and structural data

Presence of polycyclic aromatic hydrocarbons may explain apparent abundance contradictions

Abstract

Favored theories of giant planet formation center around two main paradigms, namely the core accretion model and the gravitational instability model. These two formation scenarios support the hypothesis that the giant planet metallicities should be higher or equal to that of the parent star. Meanwhile, spectra of the transiting hot Jupiter HD189733b suggest that carbon and oxygen abundances range from depleted to enriched with respect to the star. Here, using a model describing the formation sequence and composition of planetesimals in the protoplanetary disk, we determine the range of volatile abundances in the envelope of HD189733b that is consistent with the 20--80 Earth-masses of heavy elements estimated to be present in the planet's envelope. We then compare the inferred carbon and oxygen abundances to those retrieved from spectroscopy and we find a range of supersolar values that directly fit both spectra and internal structure models. In some cases, we find that the apparent contradiction between the subsolar elemental abundances and the {mass of heavy elements predicted in HD189733b by internal structure models} can be explained by the presence of large amounts of carbon molecules in the form of polycyclic aromatic hydrocarbons and soots in the upper layers of the envelope, as suggested by recent photochemical models. A diagnostic test that would confirm the presence of these compounds in the envelope is the detection of acetylene.