发表机构
State University of Tetovo; Faculdade de Ciências da Universidade de Lisboa（泰托沃国立大学; 里斯本大学理学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究基于T对偶启发的有效几何，探讨中子星内普朗克尺度正则黑洞残余，分离几何结果与吸积辐射假设，分析其热平衡、吸积时标及对中子星演化的影响，指出普朗克质量残余在中子星内基本稳定，无法在宇宙年龄内摧毁恒星。
AI 中文摘要
我们利用T对偶启发的有效几何，在中子星物质中研究普朗克尺度正则黑洞残余，并明确将几何结果与吸积和发射的假设分离开。在静态族内，表面引力温度在质量小幅增加后随$(M-M_{\rm ext})^{1/2}$增长。常数灰体斯特藩-玻尔兹曼近似给出的霍金功率与$(M-M_{\rm ext})^2$成正比，在给定假设下可产生稳定的较低平衡点和不稳定的增长阈值。然而对于$l_0=\ell_{\rm Pl}$，在单位量级的吸收效率下，形式上的较低平衡仅具有$10^{-45}$至$10^{-46}\,\mathrm{kg}$的过剩质量，因此标准描述与单个中子俘获不一致。对于具有单位系数的基准面积尺度吸收截面，平均俘获间隔为$5.4\times10^8\,\mathrm{yr}$，初始无辐射增长时标为$9.1\times10^{27}\,\mathrm{yr}$。因此在该假设下，中子星内的普朗克质量残余实际上是惰性的，若无额外供给，无法在宇宙年龄内摧毁恒星。稳态俘获-弛豫态还需要有效的微观发射定律，仅靠零温度无法确立。流体动力学吸积需要控制波效应和平均自由程判据；对于代表性物质参数，其开始对应量级为$10^{11}$至$10^{12}\,\mathrm{kg}$的质量。此处直接的零点长度修正可忽略，在飞米量级为$10^{-40}$。我们讨论了条件增长阈值、不稳定平衡附近的临界减速、暗物质供给、角动量转移以及中子星存活约束的要求。
英文摘要
We examine a Planck-scale regular black-hole remnant in neutron-star matter using a T-duality-inspired effective geometry and explicitly separate geometrical results from assumptions about absorption and emission. Within the static family, the surface-gravity temperature grows as $(M-M_{\rm ext})^{1/2}$ after a small mass increase. A constant-greybody Stefan--Boltzmann approximation gives a Hawking power proportional to $(M-M_{\rm ext})^2$ and can produce a stable lower balance point and an unstable growth threshold under stated hypotheses. For $l_0=\ell_{\rm Pl}$, however, the formal lower equilibrium has an excess mass of only $10^{-45}$--$10^{-46}\,\mathrm{kg}$ for order-unity absorption efficiency, so the canonical description is inconsistent with individual neutron captures. For a fiducial area-scale absorption cross section with unit coefficient, the mean capture interval is $5.4\times10^8\,\mathrm{yr}$ and the initial nonradiating growth timescale is $9.1\times10^{27}\,\mathrm{yr}$. Under this assumption, a Planck-mass remnant inside a neutron star is therefore effectively inert and, without additional feeding, cannot destroy the star within the age of the Universe. A stationary capture--relaxation state additionally requires an effective microscopic emission law; it is not established by zero temperature alone. Hydrodynamic accretion requires control of wave effects and a mean-free-path criterion; its onset corresponds to masses of order $10^{11}$--$10^{12}\,\mathrm{kg}$ for representative matter parameters. Direct zero-point-length corrections there are negligible, of order $10^{-40}$ at a femtometre. We discuss conditional growth thresholds, critical slowing near an unstable balance, dark-matter feeding, angular-momentum transfer, and the requirements for neutron-star survival constraints.
Comments11 pages, no figures
