Rotational velocities of the giants in symbiotic stars – I. D′‐type symbiotics★
Rotational velocities of the giants in symbiotic stars – I. D′‐type symbiotics★
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DOI：
10.1111/j.1365-2966.2005.09808.x
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发表时间：
2005-07
影响因子：
4.8
通讯作者：
R. Zamanov;M. Bode;C. Melo;J. Porter;A. Gomboc;R. Konstantinova-Antova
中科院分区：
文献类型：
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作者：
R. Zamanov;M. Bode;C. Melo;J. Porter;A. Gomboc;R. Konstantinova-Antova
我们用互相关函数方法测量了一些D '型共生星中质量施主的自转速度（vsin i）。与对应光谱类型的v sin i星表相比，五颗已知v sin i的D'共生星中有四颗似乎是非常快的自转星。这些恒星中至少有三颗以临界速度的一个相当大的分数（&0.5）旋转。这意味着至少在D '型SS中，冷的组分比孤立的巨星旋转得更快。如果这些双星是同步的，它们的轨道周期应该相对较短（4-60天）。我们还简要地讨论了快速旋转的可能起源及其与质量损失和尘埃形成的联系。
We have measured the rotational velocities (v sin i) of the mass donors in a number of D’–type symbiotic stars, using the cross-correlation function method. Four from five D’ symbiotic stars with known v sin i, appeared to be very fast rotators compared with the catalogues of v sin i for the corresponding spectral types. At least three of these stars rotate at a substantial fraction (& 0.5) of the critical velocity. This means that at least in D’–type SS the cool components rotate faster than isolated giants. If these binary stars are synchronized, their orbital periods should be relatively short (4-60 days). We also briefly discuss the possible origin of the rapid rotation and its connection with mass loss and dust formation.