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Exoplanet Albedo Spectra and Colors as a Function of Planet Phase, Separation, and Metallicity

Cahoy, Kerri L. and Marley, Mark S. and Fortney, Jonathan J. (2010) Exoplanet Albedo Spectra and Colors as a Function of Planet Phase, Separation, and Metallicity. Astrophysical Journal, 724 (1). pp. 189-214. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20160303-160615429

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Abstract

First generation space-based optical coronagraphic telescopes will obtain images of cool gas and ice giant exoplanets around nearby stars. The albedo spectra of exoplanets lying at planet-star separations larger than about 1 AU–where an exoplanet can be resolved from its parent star–are dominated by reflected light to beyond 1 µm and are punctuated by molecular absorption features. Here we consider how exoplanet albedo spectra and colors vary as a function of planet-star separation, metallicity, mass, and observed phase for Jupiter and Neptune analogs from 0.35 to 1 µm. We model Jupiter analogs with 1× and 3× the solar abundance of heavy elements, and Neptune analogs with 10× and 30× solar abundance of heavy elements. Our model planets orbit a solar analog parent star at separations of 0.8 AU, 2 AU, 5 AU, and 10 AU. We use a radiativeconvective model to compute temperature-pressure profiles. The giant exoplanets are found to be cloud-free at 0.8 AU, possess H2O clouds at 2 AU, and have both NH3 and H2O clouds at 5 AU and 10 AU. For each model planet we compute moderate resolution (R = λ/∆λ ∼ 800) albedo spectra as a function of phase. We also consider low-resolution spectra and colors that are more consistent with early direct imaging capabilities. As expected, the presence and vertical structure of clouds strongly influence the albedo spectra since cloud particles not only affect optical depth but also have highly directional scattering properties. Observations at different phases also probe different volumes of atmosphere as the source-observer geometry changes. Because the images of the planets themselves will be unresolved, their phase will not necessarily be immediately obvious, and multiple observations will be needed to discriminate between the effects of planet-star separation, metallicity, and phase on the observed albedo spectra. We consider the range of these combined effects on spectra and colors. For example, we find that the spectral influence of clouds depends more on planet-star separation and hence atmospheric temperature than metallicity, and it is easier to discriminate between cloudy 1× and 3× Jupiters than between 10× and 30× Neptunes. In addition to alkalis and methane, our Jupiter models show H2O absorption features near 0.94 µm. While solar system giant planets are well separated by their broad-band colors, we find that arbitrary giant exoplanets can have a large range of possible colors and that color alone cannot be relied upon to characterize planet types. We also predict that giant exoplanets receiving greater insolation than Jupiter will exhibit higher equator to pole temperature gradients than are found on Jupiter and thus may exhibit differing atmospheric dynamics. These results are useful for future interpretation of direct imaging exoplanet observations as well as for deriving requirements and designing filters for optical direct imaging instrumentation.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1009.3071v1arXivDiscussion Paper
http://dx.doi.org/10.1088/0004-637X/724/1/189DOIArticle
ORCID:
AuthorORCID
Marley, Mark S.0000-0002-5251-2943
Fortney, Jonathan J.0000-0002-9843-4354
Additional Information:© 2010. The American Astronomical Society. The authors thank the referee for useful comments and suggestions that improved the manuscript. We thank Richard Freedman for providing the opacity tables used in this work, and Katharina Lodders for the elemental abundances and the condensation curves. We thank Olivier Guyon for making the initial version of the PIAA coronagraph simulation available for our use. We thank Chris McKay for several useful discussions regarding the development of the radiative transfer model. K. C. is supported by an appointment to the NASA Postdoctoral Program at NASA Ames, administered by Oak Ridge Associated Universities through a contract with NASA. M. M. and J. F. acknowledge support from the NASA Planetary Atmospheres program.
Group:Keck Institute for Space Studies
Funders:
Funding AgencyGrant Number
NASA Postdoctoral ProgramUNSPECIFIED
Record Number:CaltechAUTHORS:20160303-160615429
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20160303-160615429
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:65064
Collection:CaltechAUTHORS
Deposited By: Colette Connor
Deposited On:04 Mar 2016 22:00
Last Modified:23 Aug 2017 23:41

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