拓松子：坍缩真空气泡的稳定粒子状残余
Topolons: Stable Particle-Like Remnants of Collapsed Vacuum Bubbles in a Three-Form Gauge Sector
AI总结：
研究通过Dirac-Born-Infeld作用研究四维空间中三形式规范场与带电球形膜的耦合，发现非零单极通量下坍缩气泡形成稳定残余，即拓松子，为暗物质残余提供微观解释。
摘要：
我们研究了四维时空中的三形式规范场与带电球形膜的耦合，其世界体积动力学由Dirac-Born-Infeld作用支配。四形式场强无局部传播自由度，贡献分支依赖的真空能量。受Hartle-Hawking-Wu选择论启发，我们关注 semiclassical可接受的四形式通量窗口，其中Hartle-Hawking波函数有支持。我们赋予气泡壁一个世界体积U(1)规范场，携带量化单极通量n∈Z，并评估由此产生的球形配置的完整DBI能量。我们证明能量优先分支坍缩至微观核心而非稳定在有限半径，但非零单极通量下能量在坍缩极限不消失。相反，气泡松弛为具有有限能量的残余，其质量由壁尺度和守恒通量决定。我们将这些对象解释为稳定的通量支持粒子状态，称为拓松子。在可接受的扇区中，有效能量分析区分稳定坍缩残余与对比的 runaway 真空衰减通道，从而隔离与宇宙 relic 形成相关的扇区。在宏观距离下，拓松子表现为重局域态，并提供暗物质残余的微观实现。详细的宇宙丰度和现象学留待未来工作。
英文摘要：
We study a three-form gauge sector in four spacetime dimensions coupled to electrically charged spherical membranes with Dirac--Born--Infeld (DBI) worldvolume dynamics. The associated four-form field strength has no local propagating degrees of freedom and contributes a branch-dependent vacuum energy. Motivated by the Hartle--Hawking--Wu selection argument, we restrict to the semiclassically admissible flux window and endow the membrane with a worldvolume $U(1)$ gauge field carrying quantized monopole flux $n\in\mathbb{Z}$. Evaluating the full DBI energy, we find that the energetically preferred branch collapses toward a microscopic core rather than stabilizing at finite radius. For nonzero monopole flux, however, the energy remains finite in the collapsed limit, yielding a stable flux-supported particle-like remnant whose mass is set by the wall scale and conserved flux. We call these objects topolons. Within the admissible sector, the energy analysis separates stable collapsed remnants from runaway vacuum-decay configurations, identifying the sector relevant for cosmological relic formation. At macroscopic distances, topolons behave as heavy localized states and constitute a concrete dark-relic candidate. More broadly, the construction provides the nonperturbative remnant sector of an economical three-form framework in which homogeneous four-form flux may neutralize the dominant permanent vacuum-energy contribution, while a dynamical scalar supplies the temporary positive energy required for no-boundary inflation. The detailed cosmological abundance, residual late-time vacuum energy, and phenomenology are left for future work.
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