论文标题
VLA/ALMA新生磁盘和多重性（VANDAM）对猎户座原恒星VI的调查。辐射转移建模的见解
The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars VI. Insights from Radiative Transfer Modeling
论文作者
论文摘要
我们向Markov Chain蒙特卡洛辐射转移模型进行了ALMA 345 GHz和光谱能量分布数据集，用于从VLA和ALMA新生磁盘和Orion Protostars的多重调查中的97个Protostellar磁盘样本。通过这种建模，我们为每个原始恒星得出了磁盘和包络性能，使我们能够检查年轻原恒星种群的批量性质。我们发现磁盘很小，中间的灰尘半径为$ 29.4^{+ 4.1} _ { - 2.7} $ au，中间的灰尘质量为$ 5.8^{+ 4.6} _ { - 2.7} $ M $ _ {\ oplus} $。我们发现，除包络灰尘质量和倾斜度外，I类，I和平面光谱源的大多数性质之间没有统计学上的显着差异。倾斜度之间的区别表明，0/I/flat光谱系统可能很难与Protostar的进化状态保持独特。在与类似的辐射转移模型中金牛座的II类盘尘埃质量进行比较时，我们进一步发现，磁盘尘埃质量从0级别降低到II类磁盘的趋势不再存在，尽管尚不清楚这种比较由于恒星形成区域和建模技术的差异是否公平。此外，我们建模的磁盘在广泛的重力稳定下。最后，我们将磁盘质量和半径与磁盘形成的模拟进行了比较，发现磁性水力动力学效应对于再现观察到的磁盘的特性可能很重要。
We present Markov Chain Monte Carlo radiative transfer modeling of a joint ALMA 345 GHz and spectral energy distribution dataset for a sample of 97 protostellar disks from the VLA and ALMA Nascent Disk and Multiplicity Survey of Orion Protostars. From this modeling, we derive disk and envelope properties for each protostar, allowing us to examine the bulk properties of a population of young protostars. We find that disks are small, with a median dust radius of $ 29.4^{+ 4.1}_{- 2.7}$ au and a median dust mass of $ 5.8^{+ 4.6}_{- 2.7}$ M$_{\oplus}$. We find no statistically significant difference between most properties of Class 0, I, and Flat Spectrum sources with the exception of envelope dust mass and inclination. The distinction between inclination is an indication that the Class 0/I/Flat Spectrum system may be difficult to tie uniquely to the evolutionary state of protostars. When comparing with Class II disk dust masses in Taurus from similar radiative transfer modeling, we further find that the trend of disk dust mass decreasing from Class 0 to Class II disks is no longer present, though it remains unclear whether such a comparison is fair due to differences in star forming region and modeling techniques. Moreover, the disks we model are broadly gravitationally stable. Finally, we compare disk masses and radii with simulations of disk formation and find that magnetohydrodynamical effects may be important for reproducing the observed properties of disks.
