The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. VI. Insights from Radiative Transfer Modeling
The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. VI. Insights from Radiative Transfer Modeling
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DOI：
10.3847/1538-4357/ac574d
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发表时间：
2022-02
期刊：
影响因子：
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通讯作者：
P. Sheehan;J. Tobin;L. Looney;S. Megeath
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作者：
P. Sheehan;J. Tobin;L. Looney;S. Megeath
我们提出了联合 ALMA 345 GHz 的马尔可夫链蒙特卡罗辐射传输模型以及来自 VLA 和 ALMA 新生盘以及猎户座原恒星多重巡天的 97 个原恒星盘样本的光谱能量分布数据集。从这个模型中，我们得出了每个原恒星的盘和包络特性，使我们能够检查年轻原恒星群体的整体特性。我们发现圆盘很小，中位尘埃半径为 29.4−2.7+4.1 au，中位尘埃质量为 5.8−2.7+4.6 M ⊕。我们发现，除了包络灰尘质量和倾角之外，0 类、I 类和平谱源的大多数特性之间没有统计学上的显着差异。倾角之间的区别表明，0/I/平谱系统可能很难与原恒星的进化状态唯一联系起来。当与相似的辐射传输模型中的金牛座II级盘尘埃质量进行比较时，我们进一步发现，盘状尘埃质量从0级到II级盘减少的趋势不再存在，尽管由于恒星形成区域和建模技术的差异，这种比较是否公平仍不清楚。此外，我们建模的圆盘在重力上大致稳定。最后，我们将圆盘质量和半径与圆盘形成的模拟进行比较，发现磁流体动力学效应对于再现观察到的圆盘特性可能很重要。
We present Markov Chain Monte Carlo radiative transfer modeling of a joint ALMA 345 GHz and spectral energy distribution data set 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 29.4−2.7+4.1 au and a median dust mass of 5.8−2.7+4.6 M ⊕. We find no statistically significant difference between most properties of Class 0, Class 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 owing 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.