Transmission Spectra Of Extrasolar Giant Planets In The Mid-ir

Details Transmission Spectra Of Extrasolar Giant Planets In The Mid-ir Transmission Spectra Of Extrasolar Giant Planets In The Mid-ir

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.0102t&link_type=abstract

American Astronomical Society, DPS meeting #38, #01.02; Bulletin of the American Astronomical Society, Vol. 38, p.481

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We present here simulations of transmission spectra in the mid-IR of two extrasolar giant planets, HD209458b and HD189733b, during their transit in front of their parent star (Tinetti et al., 2006). If H2O and CO are abundant as estimated by our photochemical model (Liang et al., 2004), we expect they can be detected with the IRAC and MIPS cameras on board the Spitzer Space Telescope, and with future space-based observatories, such as James Webb Space Telescope. If water vapor were far less abundant, due to a C/O ratio different from solar, other species might be observable: among them CH4, CO2 and C2H2 are the best candidates. According to our simulations, transmission spectra of EGPs in the MIR are very sensitive to molecular abundances and less to temperature. Temperature influences the spectra above all by way of its effects on the atmospheric scale height and absorption coefficients. These considerations make transmission spectroscopy, linked with primary eclipse, an approach worth considering and complementary to emission spectroscopy, linked with secondary eclipse.

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