Constraining galactic structures of mirror dark matter
Constraining galactic structures of mirror dark matter
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镜像暗物质的约束星系结构
DOI：
10.1103/physrevd.102.063518
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发表时间：
2020
影响因子：
5
通讯作者：
J. Cline
中科院分区：
文献类型：
--
作者：
Jean;J. Cline
最简单的镜面暗物质模型保持了严格的镜面对称性，但在镜面暗物质中有一个重子丰度${\mathrm{\ensuremath{\Omega}}}_{{b}^{\ensuremath{‘}}}=\ensuremath{\beta}{\mathrm{\ensuremath{\Omega}}}_{b}$和一个被抑制的温度${T}^{\ensureath{’}}=xt$，因此它只依赖于两个参数：$\ensureath{\beta}$，$x$。对于足够小的$x$，早期的宇宙学观测可能不会限制镜像重子组成所有的暗物质，尽管它们有很强的自我相互作用，这取决于隐藏部分结构形成的未知细节。在这里，我们通过模拟镜面结构的形成来填补这个漏洞，利用宇宙学和天文学数据绘制出参数空间的允许区域。我们发现，银河系磁盘表面密度和凸起质量将${\mathrm{\ensuremath{\Omega}}}_{{b}^{\ensuremath{‘}}}\ensuremath{\lesssim}0.3{\mathrm{\ensuremath{\Omega}}}_{b}$约束在BBN和CMB允许的最大值(${T}^{\ensureath{’}}=0.5T$)，或以较低的值${T}^{\${\mathrm{\ensuremath{\Omega}}}_{{b}^{\ensuremath{‘}}}\ensuremath{\lesssim}0.8{\mathrm{\ensuremath{\Omega}}}_{b}${’}}$计算。我们还简要地讨论了在我们的模型中实现SM和镜面扇区之间必要的温度不对称。
The simplest model of mirror sector dark matter maintains exact mirror symmetry, but has a baryon abundance ${\mathrm{\ensuremath{\Omega}}}_{{b}^{\ensuremath{'}}}=\ensuremath{\beta}{\mathrm{\ensuremath{\Omega}}}_{b}$ and a suppressed temperature ${T}^{\ensuremath{'}}=xT$ in the mirror sector; hence it depends only on two parameters, $\ensuremath{\beta}$, $x$. For sufficiently small $x$, early cosmological observables may not constrain mirror baryons from constituting all of the dark matter despite their strong self-interactions, depending on the unknown details of structure formation in the hidden sector. Here we close this loophole by simulating mirror structure formation, mapping out the allowed regions of parameter space using cosmological and astronomical data. We find that the Milky Way disk surface density and bulge mass constrain ${\mathrm{\ensuremath{\Omega}}}_{{b}^{\ensuremath{'}}}\ensuremath{\lesssim}0.3{\mathrm{\ensuremath{\Omega}}}_{b}$ at the highest ${T}^{\ensuremath{'}}$ allowed by BBN and CMB (${T}^{\ensuremath{'}}=0.5T$), or ${\mathrm{\ensuremath{\Omega}}}_{{b}^{\ensuremath{'}}}\ensuremath{\lesssim}0.8{\mathrm{\ensuremath{\Omega}}}_{b}$ at lower values of ${T}^{\ensuremath{'}}$. We also briefly discuss the realization of the necessary temperature asymmetry between the SM and the mirror sector in our model with unbroken mirror symmetry.
影响因子：
5
作者：
K. Nakamura;K. Hagiwara;K. Hikasa;H. Murayama;M. Tanabashi;T. Watari;C. Amsler;M. Antonelli
通讯作者：
K. Nakamura;K. Hagiwara;K. Hikasa;H. Murayama;M. Tanabashi;T. Watari;C. Amsler;M. Antonelli