新发现的中晚期Be星天鹅座V2104的多周期性
Multiperiodicity in the newly discovered mid-late Be star V2104 Cygni
摘要：
我们获得了第一个长，均匀的时间序列的V2104天鹅座，由679个数据点，与uvbybeta光度计的内华达山脉和圣佩德罗Martir天文台的目的是检测和随后解释的固有频率，这以前未研究的变星，原来是一颗Be星。我们试图找出它在主序星上部的变星B中的位置。为了获得更多的信息，我们收集了一些光谱的物理参数与ESTDIE和FIES仪器。我们使用2种不同的频率分析方法搜索UVBY通带中的频率，并使用S/N>4标准来选择显著的周期性。我们得到了估计的物理参数的基本B星的光谱类型之间的B5和B7，通过校正的存在下的拱星盘，使用的形式主义的基础上的强度的H α线发射。我们探测到3个振幅小于0.01mag的独立频率，f1 = 4.7126c/d，f2 = 2.2342c/d，f3 = 4.671c/d，发现V2104 Cyg是一颗Be星。快速旋转（vsini=290+/-10 km/s，27<i<45）阻碍了对相关脉动参数l的研究。尽管如此，对这颗中晚期Be星观测到的变化最合理的解释是非径向脉动模型。本文是根据在圣佩德罗马蒂尔国家天文台（墨西哥）、内华达山脉天文台（西班牙）、上普罗旺斯天文台（法国）获得的观测结果，以及在西班牙拉帕尔马罗克德洛斯穆查乔斯天文台的北欧光学望远镜上进行的观测结果编写的。
英文摘要：
We obtained the first long, homogenous time-series of V2104Cyg, consisting of 679 datapoints, with the uvbybeta photometers of Sierra Nevada and San Pedro Martir Observatories with the aim to detect and subsequently interpret the intrinsic frequencies of this previously unstudied variable star, which turned out to be a Be star. We try to figure out its place among the variable B stars on the upper Main Sequence. In order to obtain additional information on physical parameters we collected a few spectra with the ELODIE and FIES instruments. We searched for frequencies in the uvby passbands using 2 different frequency analysis methods and used the S/N>4 criterion to select the significant periodicities. We obtained an estimate of the physical parameters of the underlying B star of spectral type between B5 and B7, by correcting for the presence of a circumstellar disk, using a formalism based on the strenght of the Halpha line emission. We detected 3 independent frequencies with amplitudes below 0.01mag, f1 = 4.7126 c/d, f2 = 2.2342 c/d and f3 = 4.671 c/d, and discovered that V2104Cyg is a Be star. The fast rotation (vsini=290+/-10 km/s, and 27<i<45) hampered the investigation of the associated pulsational parameters l. Nevertheless, the most plausible explanation for the observed variability of this mid-late type Be star is a non-radial pulsation model. This paper is based on observations obtained at the Observatorio Astronomico Nacional San Pedro Martir (Mexico), Observatorio de Sierra Nevada (Spain), Observatoire de Haute Provence (France), and on observations made with the Nordic Optical Telescope, Observatorio Roque de los Muchachos, La Palma, Spain.
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