Volume 531, July 2011
|Number of page(s)||8|
|Section||Planets and planetary systems|
|Published online||13 June 2011|
The influence of non-isotropic scattering of thermal radiation on spectra of brown dwarfs and hot exoplanets
SRON Netherlands Institute for Space Research,
2 SUPA, School of Physics & Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS, UK
3 University of Vienna, Dpet. of Astronomy, Türkenschanzstr. 17, 1180 Vienna, Austria
4 UK Astronomy Technology Centre, Royal Observatory, Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
5 Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
Received: 4 April 2011
Accepted: 10 May 2011
Context. Currently, the thermal emission from exoplanets can be measured with either direct imaging or secondary eclipse measurements of transiting exoplanets. Most of these measurements are taken at near-infrared wavelengths, where the thermal emission of these planets peaks. Cool brown dwarfs, covering a similar temperature range, are also mostly characterised using near-infrared spectra.
Aims. We aim to show how thermal radiation in brown dwarf and exoplanet atmospheres can be scattered by clouds and haze and to investigate how the thermal emission spectrum is changed when different assumptions in the radiative transfer modelling are made.
Methods. We calculate near-infrared thermal emission spectra using a doubling-adding radiative transfer code, which includes scattering by clouds and haze. Initial temperature profiles and cloud optical depths are taken from the drift-phoenix brown dwarf model.
Results. As is well known, cloud particles change the spectrum compared to the same atmosphere with the clouds ignored. The clouds reduce fluxes in the near-infrared spectrum and make it redder than for the clear sky case. We also confirm that not including scattering in the spectral calculations can result in errors on the spectra of many tens of percent, both in magnitude and in variations with wavelength. This is especially apparent for particles that are larger than the wavelength and only have little iron in them. Scattering particles will show deeper absorption features than absorbing (e.g. iron) particles and scattering and particle size will also affect the calculated infrared colours. Large particles also tend to be strongly forward-scattering, and we show that assuming isotropic scattering in this case also leads to very large errors in the spectrum. Thus, care must be taken in the choice of radiative transfer method for heat balance or spectral calculations when clouds are present in the atmosphere. Besides the choice of radiative transfer method, the type of particles that are predicted by models will change conclusions about e.g. infrared colours and trace gas abundances. As a result, knowledge of the scattering properties of the clouds is essential when deriving temperature profiles or gas abundances from direct infrared observations of exoplanets or brown dwarfs and from secondary eclipse measurements of transiting exoplanets, since scattering clouds will change the depth of gas absorption features, among other things. Thus, ignoring the presence of clouds can yield retrieved properties that differ significantly from the real atmospheric properties.
Key words: radiative transfer / methods: numerical / planets and satellites: atmospheres / brown dwarfs / infrared: planetary systems
© ESO, 2011
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