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Absorption Spectra of the Prototype Hot-Jupiters: determination of atmospheric constituents and structure

Published online by Cambridge University Press:  01 May 2008

David K. Sing
Affiliation:
Institut d'Astrophysique de Paris, CNRS; Université Pierre et Marie Curie, 98 bis bv Arago, F-75014 Paris, France; sing@iap.fr
A. Lecavelier
Affiliation:
Institut d'Astrophysique de Paris, CNRS; Université Pierre et Marie Curie, 98 bis bv Arago, F-75014 Paris, France; sing@iap.fr
J.-M. Désert
Affiliation:
Institut d'Astrophysique de Paris, CNRS; Université Pierre et Marie Curie, 98 bis bv Arago, F-75014 Paris, France; sing@iap.fr
A. Vidal-Madjar
Affiliation:
Institut d'Astrophysique de Paris, CNRS; Université Pierre et Marie Curie, 98 bis bv Arago, F-75014 Paris, France; sing@iap.fr
G. Ballester
Affiliation:
Lunar and Planetary Laboratory, University of Arizona, Sonett Space Science Building, Tucson, AZ 85721-0063, USA
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Abstract

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The two prototype hot-Jupiter exoplanets HD209458b and HD189733b are currently offering an unprecedented view of their atmospheres. As discussed here, primary transit transmission spectra provide the opportunity to identify specific atomic and molecular species, determine their abundances, and recover temperature-pressure-altitude information. We present a reanalysis of existing HST/STIS data on HD209458b, providing a complete optical transmission spectrum. Analysis of this spectrum have revealed: (1) the planetary abundance of sodium which is ~2X solar (2) a depletion of sodium at high altitudes due to condensation or ionization (3) Rayleigh scattering by H2 (3) a high temperature at pressures of 10's mbar consistent with the dayside inversion (4) a separate high-altitude hot temperature from the planet's thermosphere and (5) likely absorption by TiO/VO. While HD209458b and HD189733b are currently the best candidates for these studies, another ~10 exoplanets are good targets with today's instruments for future transmission-based atmospheric detections.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2009

References

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