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Spitzer Secondary Eclipse Observations of Five Cool Gas Giant Planets and Empirical Trends in Cool Planet Emission Spectra | | Joshua A. Kammer
; Heather A. Knutson
; Michael R. Line
; Jonathan J. Fortney
; Drake Deming
; Adam Burrows
; Nicolas B. Cowan
; Amaury H. M. J. Triaud
; Eric Agol
; Jean-Michel Desert
; Benjamin J. Fulton
; Andrew W. Howard
; Gregory P. Laughlin
; Nikole K. Lewis
; Caroline V. Morley
; Julianne I. Moses
; Adam P. Showman
; Kamen O. Todorov
; | | Date: |
4 Aug 2015 | | Abstract: | In this work we present Spitzer 3.6 and 4.5 micron secondary eclipse
observations of five new cool (<1200 K) transiting gas giant planets:
HAT-P-19b, WASP-6b, WASP-10b, WASP-39b, and WASP-67b. We compare our measured
eclipse depths to the predictions of a suite of atmosphere models and to
eclipse depths for planets with previously published observations in order to
constrain the temperature- and mass-dependent properties of gas giant planet
atmospheres. We find that the dayside emission spectra of planets less massive
than Jupiter require models with efficient circulation of energy to the night
side and/or increased albedos, while those with masses greater than that of
Jupiter are consistently best-matched by models with inefficient circulation
and low albedos. At these relatively low temperatures we expect the atmospheric
methane to CO ratio to vary as a function of metallicity, and we therefore use
our observations of these planets to constrain their atmospheric metallicities.
We find that the most massive planets have dayside emission spectra that are
best-matched by solar metallicity atmosphere models, but we are not able to
place strong constraints on metallicities of the smaller planets in our sample.
Interestingly, we find that the ratio of the 3.6 and 4.5 micron brightness
temperatures for these cool transiting planets is independent of planet
temperature, and instead exhibits a tentative correlation with planet mass. If
this trend can be confirmed, it would suggest that the shape of these planets’
emission spectra depends primarily on their masses, consistent with the
hypothesis that lower-mass planets are more likely to have metal-rich
atmospheres. | | Source: | arXiv, 1508.0902 | | Services: | Forum | Review | PDF | Favorites | |
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