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2.5-D retrieval of atmospheric properties from exoplanet phase curves: Application to WASP-43b observations | | Patrick G.J. Irwin
; Vivien Parmentier
; Jake Taylor
; Jo Barstow
; Suzanne Aigrain
; Graham K.H. Lee
; Ryan Garland
; | | Date: |
Sat, 7 Sep 2019 09:57:10 GMT (1888kb,D) | | Abstract: | We present a novel retrieval technique that attempts to model phase curve
observations of exoplanets more realistically and reliably, which we call the
2.5-dimension (2.5-D) approach. In our 2.5-D approach we retrieve the vertical
temperature profile and mean gaseous abundance of a planet at all longitudes
and latitudes extbf{simultaneously}, assuming that the temperature or
composition, $x$, at a particular longitude and latitude $(Lambda,Phi)$ is
given by $x(Lambda,Phi) = ar{x} + (x(Lambda,0) - ar{x})cos^nPhi$,
where $ar{x}$ is the mean of the morning and evening terminator values of
$x(Lambda,0)$, and $n$ is an assumed coefficient. We compare our new 2.5-D
scheme with the more traditional 1-D approach, which assumes the same
temperature profile and gaseous abundances at all points on the visible disc of
a planet for each individual phase observation, using a set of synthetic phase
curves generated from a GCM-based simulation. We find that our 2.5-D model fits
these data more realistically than the 1-D approach, confining the hotter
regions of the planet more closely to the dayside. We then apply both models to
the WASP-43b phase curve observations of HST/WFC3 and Spitzer/IRAC (Stevenson
et al., 2017). We find that the dayside of WASP-43b is apparently much hotter
than the nightside and show that this could be explained by the presence of a
thick cloud on the nightside with a cloud top at pressure $< 0.2$ bar. We
further show that while the mole fraction of water vapour is reasonably well
constrained to $(1-10) imes10^{-4}$, the abundance of CO is very difficult to
constrain with these data since it is degenerate with temperature. | | Source: | arXiv, 1909.3233 | | Services: | Forum | Review | PDF | Favorites | |
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