用粘滞盘模型分析Be星ω CMa的V波段光变曲线
An analysis of the V-band light curve of the Be star omega CMa with the viscous decretion disk model
摘要：
我们分析了在过去四十年中观测到的Be星omega CMa的V波段测光数据。数据拟合流体动力学模型的基础上的粘性递减盘（VDD）的理论，其中一个磁盘周围的快速旋转的Be星形成的中央星和驱动器的材料喷射到逐渐更宽的轨道通过粘性扭矩。对于第一次，我们适用于磁盘建立和耗散阶段的模型。我们的模拟提供了一个很好的描述，在这两个阶段的光度变化，这表明VDD模型充分描述了磁盘结构的演变。此外，我们的分析使我们能够确定气体的粘度参数（α）以及净质量损失率。我们发现，α是可变的，范围从0.1到1.0，并建立阶段有较大的值比耗散阶段的α。此外，我们发现，与通常假设的相反，即使在静止期间，向外的质量通量也从不为零，这表明恒星在高质量损失阶段（爆发）和低质量损失阶段（静止）之间交替。
英文摘要：
We analyze the V-band photometry data of the Be star omega CMa, observed during the last four decades. The data is fitted by hydrodynamic models based on the viscous decretion disk (VDD) theory, in which a disk around a fast-spinning Be star is formed by material ejected by the central star and driven to progressively wider orbits by means of viscous torques. For the first time, we apply the model for both the disk build up and the dissipation phases. Our simulations offer a good description of the photometric variability in both phases, which suggests that the VDD model adequately describes the disk structural evolution. Furthermore, our analysis allowed us to determine the viscosity parameter (alpha) of the gas, as well as the net mass loss rate. We find that alpha is variable, ranging from 0.1 to 1.0, and that build up phases have larger values of alpha than the dissipation phases. Additionally, we find that, contrary to what is generally assumed, even during quiescence the outward mass flux is never zero, suggesting that the star alternates between a high mass-loss phase (outburst) and a low mass-loss phase (quiescence).
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