英仙座α疏散星团大范围附近的结构和运动学

Proceedings of the 48-th International student's conferences "Physics of Space" Pub Date : 1900-01-01 DOI:10.15826/b978-5-7996-2935-9.17

V. Nikiforova, M. Kulesh, A. Seleznev

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摘要

我们利用盖亚DR2星表的数据对英仙座阿尔法疏散星团(Melotte 20)的宽(大约100 × 100◦)范围进行了研究。我们在这个区域选择两个结构。第一个是星团本身，质量约为900个太阳质量，潮汐半径为12.8秒差距(4)。2◦)，日冕延伸半径约20◦。第二个是一个“流”或“丝”延伸超过70°约。这个“流”比星团稍远，并与星团部分重叠。星团和“流”的结构特征表明它们相互潮汐相互作用。我们确定了簇的旋转参数。讨论了“流”起源的不同假设。

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STRUCTURE AND KINEMATICS OF THE WIDE VICINITY OF THE ALPHA PERSEI OPEN CLUSTER

We present the results of an investigation of the wide (approximately 100 × 100 ◦ ) vicinities of the open cluster Alpha Persei (Melotte 20) by the data of the Gaia DR2 catalog. We select two structures in this region. The ﬁrst one is the cluster proper with the mass of 900 solar masses approximately and the tidal radius of 12.8 parsecs (4 . 2 ◦ ) with an extended corona with the radius of about 20 ◦ . The second one is a “stream” or the “ﬁlament” extending over 70 ◦ approximately. This “stream” is slightly farther than the cluster and overlaps with it partially. Both the cluster and the “stream” have the structural features arguing for their mutual tidal interaction. We determined the cluster rotation parameters. Diﬀerent hypothesis of the “stream” origin are discussed.

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Proceedings of the 48-th International student's conferences "Physics of Space"

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