论文标题
大气热重新分布对热jupiter的排放光谱的影响
Atmospheric heat redistribution effect on Emission spectra of Hot-Jupiters
论文作者
论文摘要
热木星是用于过境观测值的研究最多，易于检测到的系外行星。但是，仍然尚不清楚大气流与此类行星的发射光谱之间的相关性。由于热木星的昼夜温度对比很大，通过大气循环的热重分配对垂直温度压力压力结构和发射光谱有重大影响。在目前的工作中，我们旨在研究由于不同大气热重新分布而导致的温度压力曲线变化和此类行星的发射光谱的变化。为此，我们首先得出了热重新分布参数F与热木星大气层的发射通量之间的分析关系。我们在各向同性近似下的三个可能的值为1/4、1/2和2/3，分别为完整 - 再分配，半分配和无重新分配案例，并计算相应的温度压力曲线和发射光谱。接下来，我们通过使用离散空间理论形式主义来求解辐射传递方程来为F的不同值建模F的发射光谱。我们证明了大气温度压力曲线和发射光谱都易受热重新分布函数的值。热重分配的降低可导致温度压力曲线的热反转，从而增加发射通量的量。最后，我们重新审视了热木星XO-1B温度压力剖面脱落案例，并表明非反转温度压力曲线最能解释这一观察到的行星时代发射光谱。
Hot Jupiters are the most studied and easily detectable exoplanets for transit observations.However, the correlation between the atmospheric flow and the emission spectra of such planets is still not understood. Due to huge day-night temperature contrast in hot Jupiter, the thermal redistribution through atmospheric circulation has a significant impact on the vertical temperature-pressure structure and on the emission spectra. In the present work, we aim to study the variation of the temperature-pressure profiles and the emission spectra of such planets due to different amounts of atmospheric heat redistribution. For this purpose, we first derive an analytical relation between the heat redistribution parameter f and the emitted flux from the uppermost atmospheric layers of hot Jupiter. We adopt the three possible values of f under isotropic approximation as 1/4, 1/2, and 2/3 for full-redistribution, semi-redistribution and no-redistribution cases respectively and calculate the corresponding temperature-pressure profiles and the emission spectra. Next, we model the emission spectra for different values of f by numerically solving the radiative transfer equations using the discrete space theory formalism. We demonstrate that the atmospheric temperature-pressure profiles and the emission spectra both are susceptible to the values of the heat redistribution function. A reduction in the heat redistribution yields a thermal inversion in the temperature-pressure profiles and hence increases the amount of emission flux. Finally, we revisits the hot Jupiter XO-1b temperature-pressure profile degeneracy case and show that a non-inversion temperature-pressure profile best explains this observed planetary dayside emission spectra.
