tokens: 2009 ), which assumes that all LyC flux converts to unbinding the atmosphere. The LyC flux corresponds to the energy-limited mass-loss rate . In this case, the adiabatic cooling rate is and still has a less than 15% effect in the region of main concern. 8.2. Comparing with Other Hot Jupiter Upper Atmosphere Models Christie et al. ( 2013 ).—The present study agrees with the conclusion in Christie et al. ( 2013 ) that the 2 p occupation is set by radiative excitation and de-excitation, and as an improvement, we include an Ly α radiation transfer inside the atmosphere instead of applying a constant solar Ly α intensity. Because of the ∼30 times stronger stellar Ly α intensity of HD 189733 compared to the Sun and considering the Ly α photons generated inside the atmosphere owing to collisional excitation and recombination cascades, the Ly α mean intensity should be ∼100 times larger for the majority of the atomic layer. In addition, because Christie et al. ( 2013 ) underestimate n 2 p by a factor of 20 owing to a math error, n 2 p should be significantly larger in the whole simulation domain, and thus the atmosphere is optically thick to H α mainly owing to the absorption of H(2 p ). The observed H α absorption width agrees well with an optically thick atmosphere model. Because of the much larger , the photoionization of H(2 l ) is larger compared to photoionization of the ground state in the atomic layer. Hence, n e and n p in this work are ∼10 times larger. Considering the proton collisional l -mixing process with a rate ∼10 times larger than the electron collisional process, as well as the large H(2 p ) population, the creation of 2 s hydrogen is dominated by l -mixing rather than collisional excitation considered in Christie et al. ( 2013 ). As a result, 2 s and 2 p reach collisional equilibrium. In addition, it is shown that the metal lines are crucial in cooling the atmosphere. Assuming solar abundance, lines of Mg and Na can cool the atomic layer by ≃2000–3000 K. Menager et al. ( 2013 ).—Menager et al. ( 2013 ) investigate the Ly α emission and reflection by the atmosphere of HD 189733b. The temperature and electron, hydrogen, and helium number density profiles of HD 189733b from the Koskinen et al. ( 2011 ) unpublished model were applied. The temperature, n e , n p , and are in broad agreement with the profiles presented in this paper in the corresponding pressure range. According to a similar model of HD 209458b presented in Koskinen et al. ( 2013a ), it should be a one-dimensional hydrodynamic model of the upper atmosphere considering hydrogen and helium constructed on top of a full photochemical model of the lower atmosphere. They chose the average solar flux as their stellar spectrum, which is ∼10 times smaller than the synthetic spectrum from MUSCLES. Different from the photoelectron heating efficiency calculated at the fixed ionization fraction x e = 0.1 throughout the model, or a constant η applied in Koskinen et al. ( 2013a ), a
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