光解离和光电离圆盘的三维数值模拟
3D numerical simulations of photodissociated and photoionized disks
摘要：
在这项工作中，我们研究了大质量恒星的紫外辐射场对附近恒星周围的盘状气体和尘埃质量演化的影响。这个系统与猎户座的产品有相似之处。我们研究磁盘与不同的倾角和距离的来源，进行三维数值模拟。我们使用的YGUAZY-A自适应网格代码修改帐户EUV/FUV通量和非球形的质量分布。我们处理H和C的光电离再现的电离前沿和光解离区域中观察到的probrids。我们还结合了一个风的电离源，调查的弓激波的形成观察到的几个propherds。我们的研究结果表明，光蒸发风传播的磁盘表面，并成为电离后的电离锋（IF）被视为一个明亮的峰值在哈地图。我们遵循HI区域内的光蒸发风，对应于我们的大多数模型的光解区域（PDR）的发展，除了那些没有FUV通量。对于距源d \geq 0.1 pc的磁盘，PDR较厚，IF与磁盘表面分离。相比之下，对于更接近源的磁盘，PDR很薄，在我们的模拟中没有解决。IF然后与面对电离光子源的圆盘的第一网格点重合。在这两种情况下，光蒸发风冲击（IF后）与来自电离源的风，这个相互作用区域是明亮的Ha。我们的3D模型产生了两个发射特征：一个半球形的结构（与IF相关）和一个分离的弓形激波，两个风碰撞。在暴露于FUV通量的所有模型中均出现了光解离区域。更重要的是，相对于电离源具有不同倾角的圆盘具有相对相似的光解离区域。（节略）
英文摘要：
In this work we study the influence of the UV radiation field of a massive star on the evolution of a disklike mass of gas and dust around a nearby star. This system has similarities with the Orion proplyds. We study disks with different inclinations and distances from the source, performing 3D numerical simulations. We use the YGUAZÚ-A adaptative grid code modified to account for EUV/FUV fluxes and non-spherical mass distributions. We treat H and C photoionization to reproduce the ionization fronts and photodissociation regions observed in proplyds. We also incorporate a wind from the ionizing source, to investigate the formation of the bow shock observed in several proplyds. Our results show that a photoevaporated wind propagates from the disk surface and becomes ionized after an ionization front (IF) seen as a bright peak in Ha maps. We follow the development of an HI region inside the photoevaporated wind which corresponds to a photodissociated region (PDR) for most of our models, except those without a FUV flux. For disks that are at a distance from the source d \geq 0.1 pc, the PDR is thick and the IF is detached from the disk surface. In contrast, for disks that are closer to the source, the PDR is thin and not resolved in our simulations. The IF then coincides with the first grid points of the disk that are facing the ionizing photon source. In both cases, the photoevaporated wind shocks (after the IF) with the wind that comes from the ionizing source, and this interaction region is bright in Ha. Our 3D models produce two emission features: a hemispherically shaped structure (associated with the IF) and a detached bow shock where both winds collide. A photodissociated region develops in all of the models exposed to the FUV flux. More importantly, disks with different inclinations with respect to the ionizating source have relatively similar photodissociation regions. (abridged)
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