发表机构
School of Physics and Physical Engineering, Qufu Normal University（曲阜师范大学物理与光电工程学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过分析自旋原初黑洞蒸发加热星际尘埃的效应，结合次级光子贡献，推导出暗物质占比的新上限，为约束原初黑洞丰度提供了互补方法。
AI 中文摘要
原初黑洞（PBH）是一种动机良好的暗物质候选体，其宇宙丰度受到多种观测探针的约束。质量在 $10^{15}\\,\text{g}\\,{-}\\,10^{17}\\,\text{g}$ 范围内的原初黑洞目前正通过霍金辐射蒸发，这一过程可以加热星际尘埃并改变其热辐射。近期研究已利用这一效应对非自旋原初黑洞的丰度施加约束。我们通过研究原初黑洞自旋对尘埃加热约束的影响来扩展这一方法。此外，我们考虑了次级光子，这些光子不仅来源于规范玻色子的衰变，还来源于通过霍金辐射发射的初级夸克和胶子碎裂产生的强子衰变。通过将自旋原初黑洞引起的尘埃加热速率与尘埃的最大冷却速率（同时考虑硅酸盐和石墨颗粒）进行比较，我们推导出暗物质以原初黑洞形式存在的比例 $f_{\rm PBH}$ 的新上限。我们的结果表明，约束依赖于原初黑洞的质量和自旋。质量更小且自旋更高的原初黑洞产生更强的限制。例如，在我们研究的案例中，最强的约束为 $M_{\rm PBH} = 10^{15}{\rm g}$ 且自旋参数 $a_{*} = 0.9999$ 时 $f_{\rm PBH} \sim 1.5 \times 10^{-4}$。尽管这些限制不如同一质量范围内现有约束严格，但它们为约束原初黑洞丰度提供了一种独特且互补的方法。
英文摘要
Primordial black holes (PBHs) are a well-motivated dark matter candidate, and their cosmic abundance is constrained by a variety of observational probes. PBHs in the mass range $10^{15}\,\text{g}\,{-}\,10^{17}\,\text{g}$ are evaporating today via Hawking radiation, a process that can heat interstellar dust and modify its thermal emission. Recent studies have used this effect to place constraints on the abundance of non-spinning PBHs. We extend this approach by investigating the influence of PBH spin on dust-heating constraints. Furthermore, we account for secondary photons that originate not only from the decay of gauge bosons but also from the decay of hadrons produced via the fragmentation of primary quarks and gluons emitted through Hawking radiation. By comparing the dust heating rate induced by spinning PBHs with the maximum cooling rate of dust, considering both silicate and graphite grains, we derive new upper limits on the fraction of dark matter in the form of PBHs, $f_{\rm PBH}$. Our results show that the constraints depend on both PBH mass and spin. Smaller PBHs with higher spin yield stronger limits. For example, in the cases we investigated, the strongest constraint is $f_{\rm PBH} \sim 1.5 \times 10^{-4}$ for $M_{\rm PBH} = 10^{15}{\rm g}$ and spin parameter $a_{*} = 0.9999$. Although these limits are less stringent than existing constraints in the same mass range, they provide a distinct and complementary approach to constraining the abundance of PBHs.
Comments9 pages, 2 figures. A companion paper can be found at arXiv:2607.15028. comments are welcome
Journal refPhys. Rev. D 114, 063548 (2026)
