发表机构
Wuhan university（武汉大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文通过在牛顿动力学中引入正黏性系数，提出修正模型，能自然恢复MOND的深MOND极限并推导出插值函数，同时发现临界加速度随质量变化及星系缓慢膨胀等差异。
AI 中文摘要
在这项工作中，我们将一个正的黏性系数引入牛顿动力学，以探究盘状星系的旋转特性。我们的结果表明，由这种修正牛顿动力学所预言的盘状星系旋转行为，与著名的MOND模型所给出的结果具有显著的相似性。具体而言，该修正框架自然地恢复了MOND模型中假设的深MOND极限。此外，我们推导出了一个显式的插值函数，将向心加速度与牛顿加速度联系起来——这一关系在MOND模型中纯粹是经验性的。我们还指出了与MOND的关键差异：在MOND中被视为普适常数的临界加速度a0，实际上随星系质量而变化，并且对于质量更大的星系会增大。另外，受黏性系数的反耗散效应驱动，盘状星系在宇宙时间尺度上经历极其缓慢的径向膨胀，类似于宇宙的膨胀。但遗憾的是，我们尚不清楚这里引入的黏性系数的基本物理起源。不过，在现有文献中可以找到相关线索，这为我们未来的研究指明了有希望的方向。
英文摘要
In this work, we introduced a positive viscosity coefficient into Newtonian dynamics to explore the rotational properties of disk galaxies. Our results show that the rotational behaviors of disk galaxies predicted by this modified Newtonian dynamics share notable similarities with those from the well-known MOND model. Specifically, the modified framework naturally recovers the deep-MOND limit postulated in MOND. Furthermore, we derived an explicit interpolation function relating centripetal acceleration to Newtonian acceleration-a relation that is purely empirical within the MOND model. We also identify key differences from MOND: the critical acceleration a0, regarded as a universal constant in MOND, actually varies with galactic mass and increases for more massive galaxies. Additionally, driven by the anti-dissipation effect of the viscosity coefficient, disk galaxies undergo extremely slow radial expansion over cosmic time, analogous to the expansion of the Universe. But regrettably, the fundamental physical origin of the viscosity coefficient introduced here remains unclear for us. But relevant hints can be found in existing literature, pointing to a promising direction for our future research.
Comments8 pages, 3 figures
Journal refInt J Theor Phys 65, 188 (2026)
DOI：10.1007/s10773-026-06386-2
