Poster Abstracts - Kepler - NASA

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POSTER ABSTRACTSP0505. POSTER SESSION IThe Effect of Exotic Clouds on the Transmission Spectra of Transiting Super-Earths.C. V. Morley 1 , J. J. Fortney 2 , M. S. Marley 3 , C. Visscher 4 .1UC Santa Cruz, 1156 High St, Santa Cruz, CA (cmorley@ucolick.org), 2 UC Santa Cruz (jfortney@ucolick.org),NASA Ames Research Center (mark.s.marley@nasa.gov), 4Southwest Research Institute, Boulder(visscher@boulder.swri.edu).The formation of clouds in exoplanetatmospheres is expected to significantlychange the observable spectra. This is widelyunderstood for solar system planets andbrown dwarfs. For exoplanets, the gray opacityof hazes or clouds has been invoked as apossible explanation for the observed flattransmission spectrum of transiting super-Earth GJ 1214b [1]. Previous atmospheremodels for irradiated planets have includedthe most important condensates expected toform in brown dwarf and giant planet atmospheres— iron, silicate, and corundum — buthave not included the condensates expected toform at colder temperatures.The most important of these newclouds are sodium sulfide, potassium chloride,and zinc sulfide. These clouds should bemost prominent at low surface gravity,strongly super-solar atmospheric abundances,and at the slant viewing geometry appropriatefor transits. Hence they could be quite importantfor affecting the transmission spectra ofcool low density super-Earth and Neptuneclassplanets.Here, we present results from a seriesof 1D atmospheric models that include thesepreviously ignored condensates for the transitingsuper-Earths GJ 1214b and HD 97658b[2]. We vary both the metallicity of the atmosphereand the thickness of the cloudlayer, and we determine whether these exoticclouds could be sufficiently optically thick toreproduce observations of GJ 1214b.Pressure-Temperature Profiles withCondensation Curves:Pressure-Temperature profiles of transitingSuper-Earths GJ 1214b and HD 97658b areplotted with the condensation curves of allclouds expected to form. Cloud bases arelocated at the intersection between profiles andcondensation curves. Note that the pressuretemperature profiles cross the sodium sulfide,zinc sulfide, and potassium chloridecondensation curves; these clouds will form inthe upper atmosphere of both planets.[1] Bean et al. (2011) submitted to ApJ.[2] Henry et al. (2011) submitted to ApJ.1702011 Kepler Science Conference - NASA Ames Research Center
POSTER ABSTRACTSP0506. POSTER SESSION IREFRACTION OF LIGHT IN EXOPLANET ATMOSPHERES.Taishi Nakamoto 1 and Tetsuo Yamamoto 2 , 1 Tokyo Institute of Technology (Meguro, Tokyo 152-8551, Japan,nakamoto@geo.titech.ac.jp), 2 Hokkaido University (ty@lowtem.hokudai.ac.jp).Introduction: Some exoplanet atmospheres havebeen observed by transit photometry and spectroscopy.Their composition, temperature, and stratified structurehave been investigated based on those observations[e.g., 1 and references therein]. In the analyses, pathsof light that is emitted from the central star and passesthrough the atmosphere are assumed to be straight [2].In general, however, the path of light in the atmospherewould be curved due to the refraction by the atmosphere.In addition, the refraction is generally dependenton the wavelength of light. Thus, the color dependentrefraction may affect the observed quantities. If it isthe case, we would be able to obtain some informationabout the exoplanet atmosphere by observing the refraction.The refraction of light by exoplanet atmospherwas studied by [3]. In this study, we derive ahigher order analytic formula for the refraction angle,and examine the effect of refraction.Refraction Angle: We derive an analytic formulafor the refraction angle. We assume that the planetincluding the atmosphere is spherically symmetric, theatmosphere is isothermal, and the atmosphere is in thehydrostatic equilibrium. The refraction angle Θ is thengiven as,!(b,!) " 2"bH #(b)exp %$ b $ R ( +'& H )* 1+ %'3 & 2 $S (0 * b#(b)) H$ H .-0,,8b/where b is the impact parameter, ω is the frequency ofthe light, H is the scale height of the atmosphere, R isthe radius of the solid part of the planet, S 0 = 0.0858 isa constant, and Δ(b) is given by,!(b) = n2 (R)"1 #exp " b " R &% (,2 $ H 'where n(R) is the refractive index of the atmosphericgas at the bottom of the atmosphere. This formula is ahigher order one than that given by [3].Figures 1 and 2 show paths of light in the atmosphereand the refraction angle of the light obtained bynumerical calculations and the analytic formula. Inthese calculations, an Earth-like model planet is used:the radius of the solid part of the model planet and thecomposition of its atmosphere are equal to those of thecurrent Earth, and the temperature is 290K. We can seethat the light passing through the planetary atmospherecan be refracted.Figure 2: Refraction angle as a function of impactparameter.References: [1] Seager S. and Drake D. (2010)ARA&A, 48, 631–672. [2] Brown T. M. (2001) ApJ,553, 1006–1026. [3] Sidis O. and Sari R. (2010) ApJ,720, 904–911.Figure 1: Paths of light passing through the atmosphere.Green and red curves correspond to the lightwith wavelengths of 500 µm and 800 µm, respectively.Light blue curves show height from the solid surface inunit of the atmospheric scale height.2011 Kepler Science Conference - NASA Ames Research Center 171
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