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Theoretical Transmission Spectra of Exoplanet Atmospheres with Hydrocarbon Haze: Effect of Creation, Growth, and Settling of Haze Particles. II. Dependence on UV Irradiation Intensity, Metallicity, C/O Ratio, Eddy Diffusion Coefficient, and Temperature

  • Authors: Yui Kawashima, and Masahiro Ikoma

2019 The Astrophysical Journal 877 109.

  • Provider: AAS Journals

Caption: Figure 12.

Transmission spectrum models for the atmosphere with haze for the four different cases where C/O = 0.5 (green line; same as the green line in Figure 5), 1 (orange line), 10 (red line), and 1000 (purple line). The transmission spectrum for the atmosphere without haze for the case of C/O = 0.5 is also plotted (black line; same as the black line in Figure 5). As in Figure 5, the horizontal dotted lines represent the transit depths corresponding to pressure levels from 1 × 10−7 bar to 1 bar for the atmosphere in the case of C/O = 0.5. Note that the transmission spectrum models are smoothed for clarity.

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