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arXiv 1706.07029astro-ph.SR
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在二进制系统中是圆盘：II。轨道错位

Be discs in binary systems: II. Misaligned orbits

Isabelle H. Cyr, Carol E. Jones, Despina Panoglou, Alex C. Carciofi, Atsuo T. Okazaki

备注：
11 pages, 10 figures, to be published in MNRAS
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摘要：

我们使用平滑粒子流体动力学（SPH）代码来研究未对准的二进制同伴的影响，对恒星盘。我们系统地改变了光盘和双星轨道之间的错位程度，以及光盘的粘度和轨道周期，研究它们对光盘的内部和外部的密度的影响。我们发现，不同程度的错位，粘度，和轨道周期的影响截断半径和密度结构的外盘，而内盘保持大部分不受影响。我们还调查了光盘的倾斜在光盘的最里面的部分，并发现倾斜半径增加，直到达到最大值约5恒星半径。节点线的方向，相对于中心恒星的赤道，被发现是偏移相比，轨道线的节点，并在时间上周期性地变化，周期的一半轨道相位。我们还比较了我们的磁盘的分析尺度高度的等温磁盘，随着半径的$r^{1.5}$。我们发现，这个公式再现的规模高度以及对齐和错位系统，但低估了密度增强发展的光盘区域的规模高度。

英文摘要：

We use a smoothed particle hydrodynamics (SPH) code to examine the effects of misaligned binary companions on Be star discs. We systematically vary the degree of misalignment between the disc and the binary orbit, as well as the disc viscosity and orbital period to study their effects on the density in the inner and outer parts of the disc. We find that varying the degree of misalignment, the viscosity, and the orbital period affects both the truncation radius and the density structure of the outer disc, while the inner disc remains mostly unaffected. We also investigate the tilting of the disc in the innermost part of the disc and find the tilt increases with radius until reaching a maximum around 5 stellar radii. The direction of the line of nodes, with respect to the equator of the central star, is found to be offset compared to the orbital line of nodes, and to vary periodically in time, with a period of half a orbital phase. We also compare the scale height of our discs with the analytical scale height of an isothermal disc, which increases with radius as $r^{1.5}$. We find that this formula reproduces the scale height well for both aligned and misaligned systems but underestimates the scale height in regions of the disc where density enhancements develop.

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