Primordial black hole dark matter in the presence of p-wave WIMP annihilation
Primordial black hole dark matter in the presence of p-wave WIMP annihilation
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DOI：
10.1088/1475-7516/2022/03/045
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发表时间：
2021-12
影响因子：
6.4
通讯作者：
K. Kadota;H. Tashiro
中科院分区：
文献类型：
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作者：
K. Kadota;H. Tashiro
我们研究了混合暗物质场景中允许的原始黑洞 (PBH) 暗物质丰度，该混合暗物质场景由 PBH 和具有速度依赖湮没截面的自湮性弱相互作用大质量粒子 (WIMP) 组成。我们首先简要说明与熟悉的 s 波湮没场景相比，速度抑制的 p 波湮没场景中 WIMP 暗物质晕轮廓如何变化，然后讨论 PBH 质量依赖于允许的 PBH 暗物质丰度的上限。 WIMP 可以积聚到 PBH 上，形成具有尖峰密度分布的超紧凑迷你光环。这种峰值在光环的中心区域会被缓和，因为 WIMP 会被湮灭，并且这种缓和对于较小的湮灭截面来说效果较差。与 s 波湮没场景相比，速度抑制的 p 波湮没截面的 WIMP 核心密度变得更大，而核心半径变得更小。湮没截面取决于光环上变化的速度，除了 WIMP 密度分布的变化之外，另一个有趣的特征是 PBH 质量依赖于 PBH 暗物质丰度的界限。这与 s 波湮灭场景形成鲜明对比，其中 PBH 丰度范围与 PBH 质量无关。对于质量为 100 GeV 的热遗迹 p 波暗物质，允许的 PBH 暗物质分数（相对于总暗物质丰度）的量级为 f PBH ≲ 𝒪(10−7)(M⊙/MPBH)(−6+2γsp)/(3γsp+3)，其中 γsp 是尖峰轮廓的斜率指数，与 f PBH ≲ 进行比较𝒪(10−9) 用于相应的热遗迹 s 波暗物质场景。
We study the allowed primordial black hole (PBH) dark matter abundance in the mixed dark matter scenarios consisting of PBHs and self-annihilating weakly interacting massive particles (WIMPs) with a velocity dependent annihilation cross section. We first briefly illustrate how the WIMP dark matter halo profile changes for the velocity suppressed p-wave annihilation scenarios, compared with the familiar s-wave annihilation scenarios, and then discuss the PBH mass dependent upper bound on the allowed PBH dark matter abundance. The WIMPs can accrete onto a PBH to form an ultracompact minihalo with a spiky density profile. Such a spike is moderated in the central region of a halo because the WIMPs are annihilated away and this moderation is less effective for a smaller annihilation cross section. The WIMP core density becomes larger while the core radius becomes smaller for a velocity suppressed p-wave annihilation cross section than those for the s-wave annihilation scenarios. The annihilation cross section is dependent on the velocity which varies across the halo, and, in addition to the change of the WIMP density profile, another interesting feature is the PBH mass dependent bound on PBH dark matter abundance. This is in stark contrast to the s-wave annihilation scenarios where the PBH abundance bound is independent of the PBH mass. The allowed PBH dark matter fraction (with respect to the total dark matter abundance) is of order f PBH ≲ 𝒪(10−7)(M⊙/MPBH)(−6+2γsp)/(3γsp+3) for the thermal relic p-wave dark matter with the mass 100 GeV where γsp is the slope index of the spike profile, to be compared with f PBH ≲ 𝒪(10−9) for the corresponding thermal relic s-wave dark matter scenarios.