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
研究利用尘埃加热机制，通过纳入PBH自旋并考虑五种晕模型，计算光子光谱，探究对暗物质密度分布约束的依赖性，得出不同自旋参数、晕模型及质量函数下的约束结果，提供了补充性暗物质约束。
AI 中文摘要
原初黑洞（PBHs）是极具吸引力的暗物质候选者。质量在\(10^{15}\)到\(10^{18}\,\mathrm{g}\)之间的PBHs可通过霍金辐射加热星际尘埃。以往对这种尘埃加热机制的研究大多忽略PBH自旋并采用单一暗物质晕轮廓。本工作纳入PBH自旋，其显著增强辐射通量，并通过考虑五种不同晕模型系统研究对暗物质密度分布约束的依赖性。计算了包括一次和二次发射的完整光子光谱。结果表明，对于固定轮廓和质量函数，较大自旋参数对PBH分数\(f_{\mathrm{PBH}}\)产生更强约束。在晕模型中，等温轮廓给出最严格限制，其次是艾纳斯托，然后是NFW和摩尔，而布尔克特轮廓产生最弱约束。对于冷却效率低于石墨的硅酸盐颗粒，高自旋情况下上限达到\(\mathcal{O}(10^{-4})\)。考虑了单色和对数正态质量函数，发现它们之间趋势一致。对数正态情况下，较大宽度\(\sigma\)值导致排除的质量范围更广，尤其排除了大质量PBHs作为唯一暗物质成分。我们的界限通常比其他现有限制弱，但提供了补充和独立的约束。
英文摘要
Primordial black holes (PBHs) are compelling dark matter candidates. PBHs with masses between $10^{15}$ and $10^{18}\,\mathrm{g}$ can heat interstellar dust via Hawking radiation. Previous studies of this dust heating mechanism mostly neglected PBH spin and adopted a single dark matter halo profile. In this work, we incorporate PBH spin, which substantially enhances the emitted radiation flux, and systematically investigate the dependence of constraints on the dark matter density distribution by considering five different halo models. We compute the complete photon spectra, including both primary and secondary emissions. Our results show that, for a fixed profile and mass function, larger spin parameters yield stronger constraints on the PBH fraction $f_{\mathrm{PBH}}$. Among the halo models, the Isothermal profile gives the most stringent limits, followed by Einasto, then NFW and Moore, while the Burkert profile yields the weakest constraints. For silicate grains, which cool less efficiently than graphite, the upper limits reach $\mathcal{O}(10^{-4})$ for high spin cases. We consider both monochromatic and lognormal mass functions, and find consistent trends between them. For the lognormal case, larger values of the width $σ$ lead to a broader mass range being excluded, in particular ruling out massive PBHs as the sole dark matter component. Our bounds are generally weaker than other existing limits, but they provide a complementary and independent constraint.
Comments14 pages, 5 figures. new references are added. comments are welcome!
