热对流层的大气环流：具有简化强迫的HD 209458 b和HD 189733 b的三维环流模式
Atmospheric Circulation of Hot Jupiters: Three-dimensional circulation models of HD 209458b and HD 189733b with Simplified Forcing
摘要：
我们提出了全球，三维数值模拟的大气环流HD 209458 b和HD 189733 b和计算的红外光谱和光变曲线预测这些模拟，我们与现有的观测比较。辐射加热/冷却参数化与简化的牛顿松弛计划。我们的模拟开发了昼夜温度对比，随压力变化很大。在低气压（<10毫巴）下，空气从亚恒星点流向反恒星点，既沿着赤道也越过两极。在较深的层次，气流发展出一个向东的赤道急流，速度为3-4公里/秒，在高纬度地区则有较弱的向西气流。这种基本流型对模型分辨率、重力、辐射时间常数和初始温度结构的变化具有鲁棒性。夜侧光谱显示出H2O、CO和/或CH 4的深吸收带，而在昼侧，这些吸收带变平甚至翻转成发射。这是动力学对垂直温压结构的强烈影响的结果;温度在夜侧随高度强烈降低，但在昼侧几乎等温。在斯皮策带通中，我们预测的行星与恒星的通量比随着轨道相位的变化而变化2-10倍，这取决于波长和化学成分。对于HD 189733 b，其中详细的8微米光变曲线已经获得，我们正确地产生观测到的相位偏移的通量最大值，但我们不解释通量最小值，我们高估了总通量的变化。这种差异可能是由于牛顿松弛方案中固有的简化造成的，并为在未来的研究中纳入现实的辐射转移提供了动力。
英文摘要：
We present global, three-dimensional numerical simulations of the atmospheric circulation on HD 209458b and HD 189733b and calculate the infrared spectra and light curves predicted by these simulations, which we compare with available observations. Radiative heating/cooling is parameterized with a simplified Newtonian relaxation scheme. Our simulations develop day-night temperature contrasts that vary strongly with pressure. At low pressure (<10 mbar), air flows from the substellar point toward the antistellar point, both along the equator and over the poles. At deeper levels, the flow develops an eastward equatorial jet with speeds of 3-4 km/sec, with weaker westward flows at high latitudes. This basic flow pattern is robust to variations in model resolution, gravity, radiative time constant, and initial temperature structure. Nightside spectra show deep absorption bands of H2O, CO, and/or CH4, whereas on the dayside these absorption bands flatten out or even flip into emission. This results from the strong effect of dynamics on the vertical temperature-pressure structure; the temperature decreases strongly with altitude on the nightside but becomes almost isothermal on the dayside. In Spitzer bandpasses, our predicted planet-to-star flux ratios vary by a factor of 2-10 with orbital phase, depending on the wavelength and chemistry. For HD 189733b, where a detailed 8-micron light curve has been obtained, we correctly produce the observed phase offset of the flux maximum, but we do not explain the flux minimum and we overpredict the total flux variation. This discrepancy likely results from the simplifications inherent in the Newtonian relaxation scheme and provides motivation for incorporating realistic radiative transfer in future studies.
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