Giant Planet Atmospheres and Spectra

Abstract

Direct measurements of the spectra of extrasolar giant planets are the keys to determining their physical and chemical nature. The goal of theory is to provide the tools and context with which such data are understood. It is only by putting spectral observations through the sieve of theory that the promise of exoplanet research can be realized. With the new {\em Spitzer} and HST data of transiting "hot Jupiters," we have now dramatically entered the era of remote sensing. We are probing their atmospheric compositions and temperature profiles, are constraining their atmospheric dynamics, and are investigating their phase light curves. Soon, many non-transiting exoplanets with wide separations (analogs of Jupiter) will be imaged and their light curves and spectra measured. In this paper, we present the basic physics, chemistry, and spectroscopy necessary to model the current direct detections and to develop the more sophisticated theories for both close-in and wide-separation extrasolar giant planets that will be needed in the years to come as exoplanet research accelerates into its future.

in EXOPLANETS, edited by S. Seager, to be published in the Spring of 2010 in the Space Science Series of the University of Arizona Press (Tucson, AZ) (refereed)

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Cited by in corpus (4)

• Magnetic Scaling Laws for the Atmospheres of Hot Giant Exoplanets
• Photometric and Spectral Signatures of 3D Models of Transiting Giant Exoplanets
• Clouds and Hazes in Exoplanet Atmospheres
• The direct imaging search for Earth 2.0: Quantifying biases and planetary false positives