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年轻疏散星团Chi Persei和NGC 6910的集合星震学

Towards ensemble asteroseismology of the young open clusters Chi Persei and NGC 6910

S. Saesen, A. Pigulski, F. Carrier, G. Michalska, C. Aerts, J. De Ridder, M. Briquet, G. Handler, Z. Kolaczkowski, B. Acke, E. Bauwens, P. G. Beck, Y. Blom, J. … 展开作者

S. Saesen, A. Pigulski, F. Carrier, G. Michalska, C. Aerts, J. De Ridder, M. Briquet, G. Handler, Z. Kolaczkowski, B. Acke, E. Bauwens, P. G. Beck, Y. Blom, J. Blommaert, E. Broeders, M. Cherix, G. Davignon, J. Debosscher, P. Degroote, L. Decin, S. Dehaes, W. De Meester, P. Deroo, M. Desmet, R. Drummond, J. R. Eggen, J. Fu, K. Gazeas, G. A. Gelven, C. Gielen, R. Huygen, X. Jiang, B. Kalomeni, S. -L. Kim, D. H. Kim, G. Kopacki, J. -H. Kwon, D. Ladjal, C. -U. Lee, Y. -J. Lee, K. Lefever, A. Leitner, P. Lenz, A. Liakos, D. Lorenz, A. Narwid, P. Niarchos, R. Oestensen, E. Poretti, S. Prins, J. Provencal, E. Puga Antolin, J. Puschnig, G. Raskin, M. D. Reed, M. Reyniers, E. Schmidt, L. Schmitzberger, M. Spano, B. Steininger, M. Steslicki, K. Uytterhoeven, J. Vanautgaerden, B. Vandenbussche, V. Van Helshoecht, E. Vanhollebeke, H. Van Winckel, T. Verhoelst, M. Vuckovic, C. Waelkens, G. W. Wolf, K. Yakut, C. Zhang, W. Zima

备注：
4 pages, Astronomische Nachrichten, HELAS IV Conference, Arecife, Lanzarote, Feb 2010, submitted
发表信息：
Astronomische Nachrichten 331, No. 9/10, 1080 - 1083 (2010)
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摘要：

在对英仙座迟子星和NGC 6910的变星调查中，属于这两个疏散星团的Beta Cep星的数量增加到了20颗，其中9颗在NGC 6910，11颗在英仙座迟子星。我们比较脉动的属性，特别是频谱，在这两个集群的Beta Cep星，并解释集群的全球参数的差异。我们还指出，在英仙座的B型星之间的变化更复杂的图案很可能是由在这个集群中的恒星较高的自转速度。我们的结论是，两个疏散星团中的脉动星样本构成了一个很好的起点，集合星震学的β Cep型星，也可能为其他B型脉动星。

英文摘要：

As a result of the variability survey in Chi Persei and NGC6910, the number of Beta Cep stars that are members of these two open clusters is increased to twenty stars, nine in NGC6910 and eleven in Chi Persei. We compare pulsational properties, in particular the frequency spectra, of Beta Cep stars in both clusters and explain the differences in terms of the global parameters of the clusters. We also indicate that the more complicated pattern of the variability among B type stars in Chi Persei is very likely caused by higher rotational velocities of stars in this cluster. We conclude that the sample of pulsating stars in the two open clusters constitutes a very good starting point for the ensemble asteroseismology of Beta Cep-type stars and maybe also for other B-type pulsators.

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