活动双星系统UX Arietis的IUE光谱研究
A Survey of IUE Spectra of the Active Binary System UX Arietis
摘要：
为了研究明亮、不食、双线光谱双星系统UX Ari的紫外线活动，从IUE档案中获取了IUE光谱（194张图像）。在1978-1996年期间获得的光谱显示了起源于色球层和过渡区的发射线。通过比较UX Ari的UV连续谱水平与$κ$ Cet和$η$ Cep在2100 $Å$ - 3200 $Å$光谱范围内的水平，检查长波低色散光谱的紫外过量。单个Mg Ⅱ h和k发射线通量的组成星表明，G5 V和K 0 IV的系统的活动的贡献分别约为20%和80%。除了1979年1月1日观测到的耀斑事件外，在1987年、1991年和1994年也有一些通量增强，这可能表明存在7-9年的周期。对系统中紫外线过量的检查表明，UX Ari中存在一定的紫外线过量，其变化范围为1%至24%，但两张图像除外，其未显示紫外线过量。结果表明，有一个协议的来源，可以归因于磁活动的发射区。G5 V和K 0 IV组分对系统的MgII活性的贡献表明不仅需要考虑K 0 IV表面上的斑点分布，而且需要考虑UX Ari的G5 V组分表面上的斑点分布。
英文摘要：
To investigate the ultraviolet (UV) activity of the bright, non-eclipsing, double-lined spectroscopic binary system UX Ari, IUE spectra (194 images) were taken from the IUE archive. The spectra, obtained during the period 1978-1996, show emission lines originating in the chromosphere and transition region. The long-wavelength low dispersion spectra were examined for ultraviolet excess by comparing the UV continuum level of UX Ari with the levels of $κ$ Cet and $η$ Cep in the spectral range 2100 $Å$ - 3200 $Å$ . The individual MgII h and k emission-line fluxes of component stars show that the contributions to the activity of the system for G5 V and K0 IV are about 20% and 80%, respectively. Apart from the flare event observed on 1979 Jan 1, there are some flux enhancements in the years 1987, 1991 and 1994 which may suggest existence of a periodicity of about 7-9 years. Examination of the ultraviolet excess in the system showed that there is some UV excess in UX Ari, which varies from 1% up to 24% with the exception of two images which showed no UV excess. The results revealed that there was an agreement on the source of emission regions which could be attributed to the magnetic activity. The contribution of G5 V and K0 IV components to the MgII activity of the system suggests a need to take into consideration the spot distribution not only on the surface of K0 IV but also on the surface of G5 V component of UX Ari.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
