Table 3
Abundances of various species computed assuming equilibrium chemistry and solar C/O and metallicity using GGCHEM (Woitke et al. 2018) at ~1.8 × 10−1 bar.
| HD 189733b | HD 209458b | HD 97658b | Kepler-30c | |
|---|---|---|---|---|
| T (at ~1.8e-1 bar) [K] | 1353 | 1709 | 1077 | 769 |
| H2O [log VMR] | –3.5 | –3.5 | –3.7 | –3.1 |
| CO2 [log VMR] | –7.1 | –7.3 | –7.2 | –8.4 |
| CO [log VMR] | –3.4 | –3.3 | –3.6 | –6.1 |
| CH4 [log VMR] | –6.6 | –8.4 | –4.5 | –3.2 |
| NH3 [log VMR] | –7.2 | –7.7 | –6.8 | –5.5 |
| C2H2 [log VMR] | –12.3 | –12.6 | –12.0 | –17.2 |
| TiO [log VMR] | -7.1 | –6.8 | –7.9 | –10.1 |
| VO [log VMR] | -8.3 | –8.0 | –9.3 | –11.6 |
| C2H4 [log VMR] | –12.6 | –14.3 | –10.7 | –13.4 |
Notes. The temperatures given are those assumed from equilibrium chemistry forward models using ARCiS, with a self-consistently computed temperature structure, coupled with GGCHEM at this altitude of ~1.8 × 10−1 bar, an upper bound of a typical pressure layer able to be probed with transmission spectroscopy.
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