Table 1.
Parameters used for the self-consistent structure calculations for HD 179949b.
| Parameter | Value | Reference |
|---|---|---|
| T* | 6260 K | SI04 |
| R* | 1.14 R⊙ | SI04a |
| [Fe/H]* | 0.22 | SI04 |
| d | 0.045 AU | WM07 |
| MPlanet | 0.98 M♃ | BdK14 |
| RPlanet | 1.4 R♃ | b |
| Tequ | 1519 K | T*, R*, d |
| Orbital inclination i | 67.7° | BdK14 |
| Line absorbers | H2O, CO2, CO, CH4 | c |
| HCN, H2S, NH3, H2, | ||
| PH3, C2H2, OH, Na, K | ||
| Rayleigh scatterers | H2, He | c |
| CIA | H2–H2, H2–He | c |
| Elemental abundances | [Fe/H]Planet = 0.83 | d |
| Chemical abundances | Chemical equilibrium | e |
Notes. (a) The stellar radius was inferred using the stellar mass and surface gravity reported in Santos et al. (2004). (b) HD 179949b is a non-transiting planet, hence its radius is unknown. The value chosen here corresponds to the radii typically found for planets of that mass and insolation strength (see, e.g., http://exoplanets.org). (c) The references for the line opacity database of petitCODE can be found in Sect. 2.1. (d) For the solar abundances we assumed the values reported by Asplund et al. (2009). For the planet’s atmospheric enrichment the solar abundances were scaled with a value that was chosen following the method described in Sect. 4.1 of Mollière et al. (2017). (e) We used the chemical equlibrium code described in Mollière et al. (2017).
References. BdK14: Brogi et al. (2014); SI04: Santos et al. (2004); WM07: Wittenmyer et al. (2007).
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