Model Of Fluorescent Emission Of Methane In Exoplanets

Details Model Of Fluorescent Emission Of Methane In Exoplanets Model Of Fluorescent Emission Of Methane In Exoplanets

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.5605d&link_type=abstract

American Astronomical Society, DPS meeting #42, #56.05; Bulletin of the American Astronomical Society, Vol. 42, p.1079

Astronomy and Astrophysics

Astronomy

Scientific paper

Anomalous emission at 3.3 micron in the spectrum of exoplanet HD189733b has been reported in Swain et al (Nature, 2010); a possible interpretation of this suprathermal emission could be a non-LTE emission of methane induced by the strong star illumination followed by re-emission in the ν3 band complex of methane. For this purpose, a model developed for the calculation of giant planets methane fluorescence by Drossart et al. (ESA-SP427, 1999) has been adapted to the case of HD189733b to quantitatively test this interpretation. The model performs a frequency-redistributed radiative transfer model, including a five steps calculations with:
- Calculation of the absorption of stellar light by the near infrared bands of methane
- Calculation of the population of the methane vibrational levels in every atmospheric layer
- Calculation of the methane emission in the ν3 band and first two hot bands
- Self-absorption of methane emission, mostly significant for resonant fluorescence in the ν3 band
- Resonant scattering of the ν3 band self-absorption, making an additional source term in the radiative transfer equation.
The results will be presented for thermal profiles consistent with exoplanets detection, in comparison to the HD189733b spectrum observations. Implications for the modelling of exoplanets will be discussed.

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