论文标题
MIRA变量在M16-M17区域的周期变化
Period changes of Mira variables in the M16-M17 region
论文作者
论文摘要
我们使用I_C频段中的Ogle GVS数据库分析了以M16和M17之间为中心的165个AGB变量（主要是MIRA）的165个AGB变量的光曲线。与P.〜maffei使用Kodak I-N Photoghatic Plates衍生出的与已发表的光曲线的比较，使我们无法在任何恒星中找到任何重大的时期变化。值得注意的是，样品中的几颗恒星似乎已经大大改变了其平均亮度，最引人注目的情况是KZ Ser。我们为三颗星提供了更好的识别：IX Ser，NSV 10522和NSV 10326，它们都是Miras。我们将6星的光曲线分类为Maffei（Gl Ser，NSV 10271，NSV 10326，NSV 10522，NSV 10677和NSV 10772），其中五个是新的Miras，并确认V391 SCT的R CRB性质。 Maffei使用的幅度比例与现代I_C相比。
We analyzed the light curves of 165 AGB variables, mostly Miras, in the sky area centered between M16 and M17 (l=16, b=0), using the OGLE GVS database in the I_C band. Comparison with the published light curves, derived about 50 years earlier by P.~Maffei using Kodak I-N photographic plates, allowed us to find no significant period changes in any star. Remarkably, a few stars of the sample appear to have substantially changed their average luminosity, the most striking case being KZ Ser. We provide a better identification for three stars: IX Ser, NSV 10522, and NSV 10326, all of them being Miras. We classify the light curves of 6 stars, discovered but not classified by Maffei, (GL Ser, NSV 10271, NSV 10326, NSV 10522, NSV 10677, and NSV 10772) five of them being new Miras, and confirm the R CrB nature of V391 Sct. The magnitude scale used by Maffei is compared to the modern I_C one.
