The eclipsing binary V2364 Cyg is an A7V-type contact binary with a period of 0.5921 days. We presented six spectra from LAMOST and BVRc light curves (LCs), which are simultaneously analyzed to obtain the absolute physical parameters. The first light maxima are brighter than the second ones by up to 0. 038, 0. 036 and 0. 024 for BVRc bands, respectively. This distorted light curves are modeled by a cool spot on the less massive component. Its mass ratio and over-contact degree are q = 0.319(±0.004) and f = 28.4(±1.0)%. From the mass-lumonsity diagram, the primary component is a normal main-sequence star, while the secondary one is a subgiant star. From the (O−C) curve, the orbital period secularly decreases at a dP/dt = −1.62(±0.03)×10 d yr, which is mainly attributed to mass loss via stellar wind from the binary system. This may result in the observed infrared excess in the W4 band.

中文翻译：

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红外超食双星 V2364 Cyg 的光度光谱研究

食双星V2364 Cyg是一个A7V型接触双星，周期为0.5921天。我们展示了来自 LAMOST 和 BVRc 光变曲线 (LC) 的六个光谱，同时对其进行分析以获得绝对物理参数。对于 BVRc 波段，第一个光最大值比第二个光最大值分别亮 0. 038、0. 036 和 0. 024。这种扭曲的光曲线是由质量较小的组件上的冷点建模的。其质量比和过接触度为q=0.319(±0.004)和f=28.4(±1.0)%。从质量光度图中，主成分是一颗正常的主序星，而次要成分是一颗次巨星。从（OC）曲线来看，轨道周期以 dP/dt = -1.62(±0.03)×10 d yr 长期减少，这主要归因于双星系统恒星风的质量损失。