论文标题
测试WIMP暗物质模型的新方法
A new way to test the WIMP dark matter models
论文作者
论文摘要
在本文中，我们研究了通过应用最简单的现象学模型来测试弱相互作用的大粒子（WIMP）暗物质（DM）模型的可能性，该模型引入了深色能量（DE）和WIMP DM之间的相互作用项，即$ q =3γ_{DM}hρ_{dm} $。通常，耦合强度$γ_{de} $接近$ 0 $，因为de和wimp dm之间的相互作用非常弱，因此可以安全地忽略$γ_{de} $对与DM能量密度相关的$ y $演变的效果。同时，我们的数值计算还表明$ x_f \ of22 $与DM冻结温度有关，这与消失的交互情况相同。至于DM Relic密度，它将被$ \ frac {2-3γ_{dm}} {2} {2} [{2πg_* m_* m_ {dm}^3}/{（45 s_0 s_0 x_f^3}）]例如，我们分析了WIMP DM是标量DM的情况。 （SGL+SNE+Hz）和（CMB+BAO+SNE）宇宙学观察结果将给出$γ_{DM} = 0.134^{+0.17} _ { - 0.069} $和$γ_{DM} = -0.0008 \ pm0.0016 $。在进一步考虑了DM直接检测实验，DM间接检测实验和DM Relic密度的约束之后，我们发现标量DM模型的允许参数空间将被完全排除在以前的宇宙学观察结果中，而后者将增加。这两个宇宙学观察得出了几乎悖论的结论。因此，人们可能会期望在WMIP DM模型上更加严格的限制，并且在不久的将来会积累更准确的宇宙学观察。
In this paper, we investigate the possibility of testing the weakly interacting massive particle (WIMP) dark matter (DM) models by applying the simplest phenomenological model which introduces an interaction term between dark energy (DE) and WIMP DM, i.e., $Q = 3γ_{DM} Hρ_{DM}$. In general, the coupling strength $γ_{DE}$ is close to $0$ as the interaction between DE and WIMP DM is very weak, thus the effect of $γ_ {DE}$ on the evolution of $Y$ associated with DM energy density can be safely neglected. Meanwhile, our numerical calculation also indicates that $x_f\approx20$ is associated with DM freeze-out temperature, which is the same as the vanishing interaction scenario. As for DM relic density, it will be magnified by $\frac{2-3γ_{DM}}{2}[{2πg_* m_{DM}^3}/{(45 s_0 x_f^3})]^{γ_{DM}}$ times, which provides a new way to test WIMP DM models. As an example, we analyze the case in which WIMP DM is a scalar DM. (SGL+SNe+Hz) and (CMB+BAO+SNe) cosmological observations will give $γ_{DM}=0.134^{+0.17}_{-0.069}$ and $γ_{DM}=-0.0008\pm0.0016$, respectively. After further considering the constraints from DM direct detection experiment, DM indirect detection experiment, and DM relic density, we find that the allowed parameter space of the scalar DM model will be completely excluded for the former cosmological observations, while it will increase for the latter ones. Those two cosmological observations lead to an almost paradoxical conclusion. Therefore, one could expect more stringent constraints on the WMIP DM models, with the accumulation of more accurate cosmological observations in the near future.
