TRANSMISSION SPECTRA OF THREE-DIMENSIONAL HOT JUPITER MODEL ATMOSPHERES

被引:242
作者
Fortney, J. J. [1 ]
Shabram, M. [1 ]
Showman, A. P. [2 ]
Lian, Y. [2 ]
Freedman, R. S. [3 ,4 ]
Marley, M. S. [3 ]
Lewis, N. K. [2 ]
机构
[1] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA
[2] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA
[3] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA
[4] SETI Inst, Mountain View, CA 94043 USA
关键词
planetary systems; radiative transfer; stars:; individual; (HD; 209458; HD; 189733); EXTRASOLAR GIANT PLANETS; EXOPLANET HD 189733B; MASS DWARF STARS; GENERAL-CIRCULATION MODEL; HUBBLE-SPACE-TELESCOPE; CARBON-MONOXIDE; THERMAL EMISSION; LIGHT CURVES; MU-M; CHEMICAL-EQUILIBRIUM;
D O I
10.1088/0004-637X/709/2/1396
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We compute models of the transmission spectra of planets HD 209458b, HD 189733b, and generic hot Jupiters. We examine the effects of temperature, surface gravity, and metallicity for the generic planets as a guide to understanding transmission spectra in general. We find that carbon dioxide absorption at 4.4 and 15 mu m is prominent at high metallicity, and is a clear metallicity indicator. For HD 209458b and HD 189733b, we compute spectra for both one-dimensional and three-dimensional model atmospheres and examine the differences between them. The differences are usually small, but can be large if atmospheric temperatures are near important chemical abundance boundaries. The calculations for the three-dimensional atmospheres, and their comparison with data, serve as constraints on these dynamical models that complement the secondary eclipse and light curve data sets. For HD 209458b, even if TiO and VO gases are abundant on the dayside, their abundances can be considerably reduced on the cooler planetary limb. However, given the predicted limb temperatures and TiO abundances, the model's optical opacity is too high. For HD 189733b we find a good match with some infrared data sets and constrain the altitude of a postulated haze layer. For this planet, substantial differences can exist between the transmission spectra of the leading and trailing hemispheres, which are an excellent probe of carbon chemistry. In thermochemical equilibrium, the cooler leading hemisphere is methane-dominated, and the hotter trailing hemisphere is CO-dominated, but these differences may be eliminated by non-equilibrium chemistry due to vertical mixing. It may be possible to constrain the carbon chemistry of this planet, and its spatial variation, with James Webb Space Telescope.
引用
收藏
页码:1396 / 1406
页数:11
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