2019ApJ...880...90Y

Because mass-loss rates are the function of the mean density of a planet and the stellar irradiation, we calculated about 450 models covering planets with different densities and stellar irradiation. Our results show that the mass-loss rates are dependent on the stellar irradiation and the mean density. However, the mass-loss rates predicted by the energy-limited equation are higher than those predicted by the hydrodynamic model when the integrated extreme ultraviolet flux is higher than ∼2 x 10⁴ erg cm^–2 s^–1. The overestimation can be revised if the kinetic and thermal energies of the escaping atmosphere is included in the energy-limited equation. We found that the heating efficiencies are proportional to the product of the gravitational potential of the planet and the stellar irradiation. The mean absorption radii of stellar irradiation are 1.1-1.2 R_p for Jupiter-like planets, while they vary in the range of 1.1-1.7 R_p for planets with smaller sizes. We evaluated the absorption of stellar Lyα by the planetary atmosphere and found that the deeper Lyα absorptions tend to be located in the high stellar irradiation and low planetary mean density regions, and vice versa. Moreover, planets with mass-loss rates higher than 10¹¹ g s^–1 are likely to exhibit obvious absorptions. Finally, we suggest that the absorption levels are related to the inherent properties of exoplanets. The planets with larger sizes (or lower mean density) show strong Lyα absorptions. Neptune-like and Earth-like planets tend to have weak Lyα absorptions because of their small sizes (or high densities).