Radiative transfer in protoplanetary disks under irradiation by the protostar
Radiative transfer in protoplanetary disks under irradiation by the protostar
复制标题
原恒星照射下原行星盘的辐射传输
DOI：
10.1093/ptep/ptt028
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发表时间：
2013
期刊：
影响因子：
--
通讯作者：
Jun Fukue
中科院分区：
文献类型：
--
作者：
Kato;他2名;Jun Fukue
在考虑各向异性散射效应的非Gray频率相关处理下，研究了原恒星辐照下原行星吸积盘中的辐射传输。由于辐射加热，盘被分成内部光学厚的平坦盘、中间光学厚的喇叭形盘和外部光学薄的喇叭形盘。在每一个制度下，出射强度以及其他辐射量的爱丁顿近似下解析获得。在内部平坦的磁盘，磁盘是光学厚和粘性加热占主导地位，我们得到的垂直均匀加热的情况下的解决方案。在中间爆发的磁盘，磁盘是光学厚和几何爆发由于辐射加热，我们得到的解决方案的局部热力学平衡（LTE）的情况下，假设一个线性普朗克函数。在外部喇叭形磁盘，其中磁盘是光学薄和喇叭形由于辐射加热，我们得到的LTE情况下的垂直等温磁盘的解决方案。的温度结构是一致的，在以前的研究中所看到的，而磁盘强度是不同的，从以前的情况下，没有各向异性散射。我们发现，各向异性散射增强出射强度在极向方向，当前向散射占主导地位。因此，除了通常的边缘变暗效应外，原行星盘在极向方向也变得明亮。
Radiative transfer in a protoplanetary accretion disk, which is irradiated by the protostar, is examined under the non-gray frequency-dependent treatment, including the anisotropic scattering effect. Due to irradiation heating, the disk is divided into an inner optically thick flat disk, a middle optically thick flared disk, and an outer optically thin flared disk. In each regime, emergent intensities as well as other radiative quantities are analytically obtained under the Eddington approximation. In the inner flat disk, where the disk is optically thick and viscous heating is dominant, we obtain solutions for the case of vertically uniform heating. In the middle flared disk, where the disk is optically thick and geometrically flared due to irradiation heating, we obtain solutions for the local thermodynamic equilibrium (LTE) case under the assumption of a linear Planck function. In the outer flared disk, where the disk is optically thin and flared due to irradiation heating, we obtain solutions for the LTE case of a vertically isothermal disk. The temperature structure is consistent with that seen in previous studies, while disk intensities are different from those in previous cases without anisotropic scattering. We found that anisotropic scattering enhances the emergent intensity in the poleward direction, when forward scattering dominates. As a result, in addition to the usual limb-darkening effect, the protoplanetary disk also becomes bright in the poleward direction.