发表机构
Universidad Nacional Autónoma de México. Instituto de Astronomía（墨西哥国立自治大学天文学研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文综合观测与模拟，研究了长周期激变变星V630 Cas，揭示其非轴对称进动盘结构，并估算供体质量约0.38 Ms，通过MESA演化模拟解释了其性质。
AI 中文摘要
我们对V630 Cassiopeiae进行了全面综述，这是一颗周期非常长的激变变星。基于结合TESS提供的光谱和高分辨率测光以及GAIA提供的精确距离数据的新观测，我们确认并扩展了先前描述的特征。光变曲线在不同历元之间表现出不同的行为，这归因于盘亮度分布的变化，可能是由于非轴对称结构（如进动的偏心盘）所致。光谱分析揭示了复杂的Hα线轮廓，具有双成分和发射分布，表明存在一个大的、不对称的、可能进动的盘，而非物质流撞击区域中的经典激波结构。多普勒层析成像表明，发射起源于盘的边缘，呈不对称分布而非紧凑的点，这使得径向速度的解释复杂化，并限制了其用于精确确定质量的能力。通过测光和光谱分析，我们在采用的2409 pc距离下建立了供体质量估计，近似值为0.38 Ms，但存在与距离及其他系统因素相关的显著不确定性。最后，利用V630 Cas的参数，使用包含CARB磁制动方案的MESA进行了双星演化模拟，以确定一个能够解释其性质的演化序列。
英文摘要
We present a comprehensive review of V630 Cassiopeiae, which is a very long-period cataclysmic variable. Based on new observations combining spectroscopy and high-resolution photometry provided by TESS and precise distance data from GAIA, we confirm and extend previously described characteristics. The light curves show differential behaviors between different epochs, attributed to changes in the disk's brightness distribution, likely due to non-axial structures such as precessing eccentric disks. The spectroscopy reveals complex Ha line profiles, with dual components and an emission distribution that suggests a large, asymmetric, and possibly precessing disk, rather than a classic shock structure in the matter-flow impact region. Doppler tomography indicates that the emission originates at the periphery of the disk, distributed in an asymmetric pattern rather than a compact point, complicating the interpretation of radial velocities and limiting their use for accurately determining masses. Through photometric and spectroscopic analysis, we established a donor mass estimate with an approximate value of 0.38 Ms at the adopted distance of 2409 pc, with significant uncertainty related to distance and other systematic factors. Finally, using the parameters of V630 Cas, binary evolution simulations were conducted with MESA incorporating CARB magnetic braking prescription to identify an evolutionary sequence that explains its properties.
Comments18 pages, 14 figures to appear in RMxAA
