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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 15.

Transmission spectrum models for the atmosphere with haze for the three different cases where Kzz = 1 × 109 cm2 s−1 (light-blue line), Kzz = 1 ×107 cm2 s−1 (green line; same as the green line in Figure 5), and Kzz = 1 ×105 cm2 s−1 (purple line). The transmission spectrum for the atmosphere without haze for the case of Kzz = 1 × 107 cm2 s−1 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 × 10−6 bar to 1 bar for the atmosphere in the case of Kzz = 1 × 107 cm2 s−1. Note that the transmission spectrum models are smoothed for clarity.

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