Vev触发器：暗物质在弱尺度相变之间的衰变
The Vev Flip-Flop: Dark Matter Decay between Weak Scale Phase Transitions
摘要：
我们提出了一个新的替代弱相互作用大质量粒子（WIMP）的暗物质范例。在这种情况下，暗物质丰度不是由热冻结决定的，而是由暗物质衰变决定的，这是在电弱相变之前的有限时间内允许的。更具体地说，我们考虑费米单线态暗物质粒子弱耦合到标量介体$S_3$和辅助暗扇区字段，收费下的标准模型规范群。暗物质在仍处于相对论性时就被冻结了，所以它的丰度最初非常大。随着宇宙冷却下来，标量介质产生真空期望值（vev），这打破了稳定暗物质的对称性。这使得暗物质与带电费米子混合并衰变。在这一时期，暗物质丰度减少到今天观测到的值。之后，SM希格斯场也发展出一个vev，它反馈到$S_3$势中，恢复了暗扇区的对称性。在一个具体的模型中，我们表明，这种“vev触发器”的情况下是现象上成功的参数空间中最有趣的区域。我们还评论在大型强子对撞机和其他地方的检测前景。
英文摘要：
We propose a new alternative to the Weakly Interacting Massive Particle (WIMP) paradigm for dark matter. Rather than being determined by thermal freeze-out, the dark matter abundance in this scenario is set by dark matter decay, which is allowed for a limited amount of time just before the electroweak phase transition. More specifically, we consider fermionic singlet dark matter particles coupled weakly to a scalar mediator $S_3$ and to auxiliary dark sector fields, charged under the Standard Model gauge groups. Dark matter freezes out while still relativistic, so its abundance is initially very large. As the Universe cools down, the scalar mediator develops a vacuum expectation value (vev), which breaks the symmetry that stabilises dark matter. This allows dark matter to mix with charged fermions and decay. During this epoch, the dark matter abundance is reduced to give the value observed today. Later, the SM Higgs field also develops a vev, which feeds back into the $S_3$ potential and restores the dark sector symmetry. In a concrete model we show that this "vev flip-flop" scenario is phenomenologically successful in the most interesting regions of its parameter space. We also comment on detection prospects at the LHC and elsewhere.
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