A GENERAL CIRCULATION MODEL FOR GASEOUS EXOPLANETS WITH DOUBLE-GRAY RADIATIVE TRANSFER
A GENERAL CIRCULATION MODEL FOR GASEOUS EXOPLANETS WITH DOUBLE-GRAY RADIATIVE TRANSFER
复制标题
具有双灰辐射传输的气态系外行星的一般环流模型
DOI：
10.1088/0004-637x/750/2/96
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
K. Menou
中科院分区：
文献类型：
--
作者：
E. Rauscher;K. Menou
我们提出了一个新版本的我们的代码为气态系外行星的大气环流建模，现在采用了“双灰”辐射传输方案，自洽解决整个大气中的通量和加热，包括新兴的（可观察到的）红外通量。我们将辐射分为红外和光学分量，每个分量都有自己的吸收系数，并求解标准的双流辐射传输方程。我们使用恒定的光吸收系数，而红外系数可以与压力成幂律关系;然而，为了简单起见，本文所示的结果使用恒定的红外系数。在这里，我们将详细描述我们的新代码，并通过介绍一个通用的热木星模型来演示其实用程序。我们讨论的问题有关的建模最深的大气压力，并描述我们使用的扩散近似在高光学深度的辐射通量。此外，我们提出了新的模型，使用一个简单的形式对大气的磁阻力。我们计算了发射的热相位曲线，发现我们的无拖曳模型的大气最亮区域与亚恒星点的偏移量为0.12 °，最小通量为最大通量的17%，而具有最强磁拖曳的模型的偏移量仅为0.12 °，比值为13%。最后，我们计算了每个模型的动能数值损失率，除了我们的强阻力模型，那里没有可测量的损失;我们推测这是由于该模型中的风速大大降低。
We present a new version of our code for modeling the atmospheric circulation on gaseous exoplanets, now employing a “double-gray” radiative transfer scheme, which self-consistently solves for fluxes and heating throughout the atmosphere, including the emerging (observable) infrared flux. We separate the radiation into infrared and optical components, each with its own absorption coefficient, and solve standard two-stream radiative transfer equations. We use a constant optical absorption coefficient, while the infrared coefficient can scale as a power law with pressure; however, for simplicity, the results shown in this paper use a constant infrared coefficient. Here we describe our new code in detail and demonstrate its utility by presenting a generic hot Jupiter model. We discuss issues related to modeling the deepest pressures of the atmosphere and describe our use of the diffusion approximation for radiative fluxes at high optical depths. In addition, we present new models using a simple form for magnetic drag on the atmosphere. We calculate emitted thermal phase curves and find that our drag-free model has the brightest region of the atmosphere offset by ∼12° from the substellar point and a minimum flux that is 17% of the maximum, while the model with the strongest magnetic drag has an offset of only ∼2° and a ratio of 13%. Finally, we calculate rates of numerical loss of kinetic energy at ∼15% for every model except for our strong-drag model, where there is no measurable loss; we speculate that this is due to the much decreased wind speeds in that model.
热行星大气流动模拟中的弛豫时间和耗散相互作用
DOI：
10.1088/0004-637x/729/2/117
发表时间：
2011
期刊：
The Astrophysical Journal
影响因子：
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作者：
Thrastarson H
通讯作者：
Thrastarson H