Abstract Cataclysmic Variables (CVs) are compact binaries with white dwarf (WD) primaries. CVs and other accreting WD binaries (AWBs) are useful laboratories for studying accretion flows, gas dynamics, outflows, transient outbursts, and explosive nuclear burning under different astrophysical plasma conditions. They have been studied over decades and are important for population studies of galactic X-ray sources. Recent space- and ground-based high resolution spectral and timing studies, along with recent surveys indicate that we still have observational and theoretical complexities yet to answer. I review accretion in nonmagnetic AWBs in the light of X-ray observations. I present X-ray diagnostics of accretion in dwarf novae and the disk outbursts, the nova-like systems, and the state of the research on the disk winds and outflows in the nonmagnetic CVs together with comparisons and relations to classical and recurrent nova systems, AM CVns and Symbiotic systems. I discuss how the advective hot accretion flows (ADAF-like) in the inner regions of accretion disks (merged with boundary layer zones) in nonmagnetic CVs explain most of the discrepancies and complexities that have been encountered in the X-ray observations. I stress how flickering variability studies from optical to X-rays can be probes to determine accretion history and disk structure together with how the temporal and spectral variability of CVs are related to that of LMXBs and AGNs. Finally, I discuss the nature of accretion in nonmagnetic WDs in terms of ADAF-like accretion flows, and elaborate on the solutions it brings and its complications, constructing an observational framework to motivate new theoretical calculations that introduce this flow-type in disks, outflow and wind models together with disk-instability models of outbursts and nova outbursts in AWBs and WD physics, in general.

中文翻译：

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在 X 射线中观察到的非磁性白矮星双星中的吸积流

摘要 Cataclysmic Variables (CVs) 是具有白矮星 (WD) 主星的紧凑双星。CV 和其他吸积 WD 双星 (AWB) 是研究吸积流、气体动力学、流出、瞬态爆发和不同天体物理等离子体条件下爆炸性核燃烧的有用实验室。它们已经被研究了几十年，对于银河 X 射线源的群体研究很重要。最近的空间和地面高分辨率光谱和时间研究以及最近的调查表明，我们仍然有观测和理论的复杂性尚未回答。我根据 X 射线观察回顾了非磁性 AWB 中的吸积。我展示了矮新星吸积和圆盘爆发的 X 射线诊断，类新星系统，以及对非磁性 CV 中圆盘风和流出的研究状态，以及与经典和循环新星系统、AM CVns 和共生系统的比较和关系。我讨论了非磁性 CV 中吸积盘内部区域（与边界层区域合并）的平流热吸积流（类似 ADAF）如何解释 X 射线观测中遇到的大多数差异和复杂性。我强调了从光学到 X 射线的闪烁变异性研究如何成为确定吸积历史和盘结构的探针，以及 CV 的时间和光谱变异性与 LMXB 和 AGN 的时间和光谱变异性之间的关系。最后，我根据类似 ADAF 的吸积流讨论了非磁性 WD 中吸积的性质，并详细阐述了它带来的解决方案及其复杂性，