Exoclimes_Conference_booklet1

Finally, we will show GCM simulations coupling the 3D dynamical core to this radiative
model, and discuss the large-scale stratospheric circulations driven by the radiative
forcing.
Simulated transit spectra of Earth and Jupiter
Patrick Irwin — University of Oxford
In recent years, increasingly accurate measurements have been made of the transit
spectra of hot Jupiters, such as HD 189733b, from the visible through to mid-infrared
wavelengths. These have been modelled to derive the likely atmospheric structure and
composition of these planets. As measurement techniques improve, the transit spectra of
super-Earths such as GJ 1214b are becoming increasingly accessible, allowing model
atmospheric states to be fitted for this class of planet also. While it is not yet possible to
constrain the atmospheric states of solar system-like planets such as the Earth or Jupiter
from such measurements, it is hoped that this might one day become practical; if so, it is of
interest to determine what we might infer from such measurements. In this work we have
constructed atmospheric models of Earth and Jupiter from 0.2 - 15 microns that are
consistent with ground-based and satellite observations. From these models we calculate
the primary and secondary transit spectra (with respect to the Sun) that would be observed
by a remote observer, many light years away, and also directly imaged spectra, assuming
that this one day becomes technically feasible. From these spectra we test how well
optimal estimation retrieval models can determine the atmospheric states and compare
these with the “ground truths” in order to assess: a) the inherent difficulty in using transit
spectra observations to observe solar system-like targets; b) the relative merits of primary
versus secondary transit spectra; and c) the optimal wavelength coverage, resolutions and
sensitivities required to retrieve useful information about the atmospheres of such planets.
D/H ratios in methane in the atmosphere of giant planets and Titan!
Lucyna Kedziora-Chudczer — University of New South Wales
We present observations of the GNIRS/GEMINI high resolution spectra at 1.58 and 2.03
microns for the giant planets of our Solar System and Saturn's moon Titan. We fitted the
atmospheric absorption spectra of these objects using the VSTAR line-by-line radiative
transfer modelling to estimate the D/H ratios from deuterated methane in both bands.
Deuteration of the outer planets can be used not only as a diagnostic of initial conditions in
the solar nebula during formation of giant planets but also to help to determine the location
at which planets accreted the bulk of their mass. We estimated that based on D/H ratio
derived for Titan, the Saturnian system formed close to its current location, which has
implication on previously proposed migration theories.
Vertical structure of gas-planet atmospheres inferred from methane bands
Nadiia Kostogryz — Kiepenheuer-Institut für Sonnenphysik
Visible and near infrared spectra of the Jovian planets in the Solar system are dominated
by methane absorption features. These bands are very useful for determining the vertical
cloud structure of planetary atmospheres as was proposed by Morozhenko (1984) and
implemented for the Uranus atmosphere by Kostogryz (2013). The fact that the diffusely
reflected radiation is formed at different effective depths in the atmosphere allows to
constrain the vertical cloud structure. The cloud height and opacity strongly influence the
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