论文标题
加热Peccei-Quinn量表
Heating up Peccei-Quinn scale
论文作者
论文摘要
我们在新的情况下讨论了QCD Axion暗物质的产生，该方案假设Peccei-Quinn对称性破裂的时间变化。后者随着宇宙在早期的温度而下降，最终以较大的恒定值稳定。这种行为是由携带Peccei-Quinn电荷的复杂场与类似Higgs的标量（与原始等离子体的热平衡中的）相互作用引起的。在这种情况下，轴是在复杂的Peccei-Quinn场的参数共振衰减中有效产生的，在辐射主导的阶段放松至最小值。值得注意的是，此过程不受宇宙的膨胀率的影响，并允许独立于轴突质量产生所需的深色物质。模型参数空间上的现象学约束取决于径向场波动的数量密度，这些密度也与轴相同，并且在原始等离子体中的热速率也是如此。 For the ratio of radial field and axion particles number densities larger than $\sim 0.01$ at the end of parametric resonance decay, the combination of cosmological and astrophysical observations with the CAST limit confines the Peccei-Quinn scale to a narrow range of values $\sim 10^{8}~\mbox{GeV}$, - this paves the way for ruling out our scenario with the near未来搜索斧头。
We discuss production of QCD axion dark matter in a novel scenario, which assumes time-varying scale of Peccei-Quinn symmetry breaking. The latter decreases as the Universe's temperature at early times and eventually stabilises at a large constant value. Such behavior is caused by the portal interaction between the complex field carrying Peccei-Quinn charge and a Higgs-like scalar, which is in thermal equilibrium with primordial plasma. In this scenario, axions are efficiently produced during the parametric resonance decay of the complex Peccei-Quinn field, relaxing to the minimum of its potential in the radiation-dominated stage. Notably, this process is not affected by the Universe's expansion rate and allows to generate the required abundance of dark matter independently of an axion mass. Phenomenological constraints on the model parameter space depend on the number density of radial field fluctuations, which are also generically excited along with axions, and the rate of their thermalization in the primordial plasma. For the ratio of radial field and axion particles number densities larger than $\sim 0.01$ at the end of parametric resonance decay, the combination of cosmological and astrophysical observations with the CAST limit confines the Peccei-Quinn scale to a narrow range of values $\sim 10^{8}~\mbox{GeV}$, - this paves the way for ruling out our scenario with the near future searches for axions.
