Exoclimes_Conference_booklet1

atios, and temperature profiles, that might be important clues to their formation and
evolution.
Models of exoplanet evaporation
James! Owen — Canadian Institute for Theoretical Astrophysics
Given the numerous exoplanets discovered at close separations to their parents stars,
where the stellar UV & X-ray radiation fields can heat the upper layers of the planets
atmosphere to 10 4 K, evaporation is bound to occur. I will discuss evaporation in the
hydrodynamic limit which can be driven by either the EUV or X-ray radiation, and the
associated mass-loss rates. I will argue that evaporation of close-in exoplanets does not
occur in `energy-limited' sense where PdV work dominates the energy loss, but that
radiative cooling and recombinations are dominant energy sinks. Finally, I will present the
results of multi-dimensional calculations and discuss the role planetary and stellar
magnetic fields play in exoplanet evaporation, along with the long term impact of
evaporation on exoplanets.
Transit Transmission spectroscopy with GTC: First results
Enric Palle — Instituto de Astrofisica de Canarias
Our group is presently conducting an observational campaign, using the 10-meter Gran
Telescopio Canarias (GTC), to obtain long-slit spectra in the optical range of several
planetary host stars (and a reference star) during a transit event. The GTC instrument
OSIRIS consists of two CCD detectors with a field of view of 7.8 X 7.8 arcmin. We used
OSIRIS in its long-slit spectroscopic mode, selecting the grism R=1000 which covers the
spectral range of 520-1040 nm, and a custom-built slit of 12 arcsec of width. A Markov
Chain Monte Carlo (MCMC) Bayesian approach is used for the transit fitting, and the level
of red noise in the light curves is estimated using the method of Winn et al. (2008). Here,
we will present refined planet parameters, planet color signatures, and the transmission
spectrum of a set of know transiting exoplanets, namely: WASP-43b, HAT-P-12b,
WASP-48b, and KIC 12557548b. With our instrumental setup, GTC has been able to
reach precision down to 250 ppm (WASP-48b, V=11.06 mag) for each color light curve 15
nm wide. We will also discuss the capabilities and advantages of GTC as tool for the
follow up of faint Kepler targets, such as KIC 12557548b. The light curves obtained for this
object with low resolution gratings allow us to reach 300 ppm in a 4-min sampled curve,
thus revealing the detailed shape, small scale structures, and color information of
individual transits of KIC12557548b.
Characterisation of exoplanet atmospheres with KMOS
Hannu Parviainen — University of Oxford
We present our preliminary results and experiences with the KMOS (K-Band Multi-Object
Spectrometer) instrument in the characterisation of exoplanet atmospheres using transit
transmission spectroscopy, and detail our approach to the data reduction and analysis.
Our experiences are mainly based on transits observed during the instrument's
commissioning phase, and the investigation of the KMOS instrument's applicability to
transit spectroscopy was an important secondary goal along with the science driver.
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