论文标题
低表面亮度星系中暗物质状态的可能方程
The Possible Equation Of State Of Dark Matter in Low Surface Brightness Galaxies
论文作者
论文摘要
观察到的低表面亮度（LSB）星系的旋转曲线在研究暗物质中起着至关重要的作用，并表明存在一个中央恒定密度暗物质核心。但是，冷暗物质的宇宙n体仿真预测了具有幂律质量密度分布的内部脉管halo，并且无法再现中央恒定密度核心。这种现象称为尖核问题。当暗物质静止并满足静液压平衡的条件时，使用状态方程可以在静态和球形对称时空中获得密度曲线。为了解决尖峰核问题，我们假设状态方程与缩放转换无关。这种类型的状态方程式的较低顺序近似自然会导致特殊情况，即$ p =ζρ+2εv_{rot}^{2}ρ$，其中$ p $和$ p $是压力和密度，$ v_ {rot} $是Galaxy of Galaxy of Galaxy of Galaxy of Galaxy of Galaxy of Galaxy of Galaxy，$ $ $ $ζ$和榜单。当$ε$约为$ 0.15 $时，它可以获得与伪静脉光环型相似的密度曲线。要获取一个更广泛的模型，让状态方程包括多面性模型，即$ p = \fracζ{ρ_{ρ_{0}^{s}}ρ{1+ s}+ s}+ s}+ s}+ s}+ s}+2εv_{rot}^{2}^{2}ρ{2}ρ$，我们可以与$相同的profiles，例如$ s的$ s，例如，$ s相同，$ s的$ s n ys $ s s ys $ s ys $ s ys $ she $ s。 $ρ_{0} $是正常数。
The observed rotation curves of low surface brightness (LSB) galaxies play an essential role in studying dark matter, and indicate that there exists a central constant density dark matter core. However, the cosmological N-body simulations of cold dark matter predict an inner cusped halo with a power-law mass density distribution, and can't reproduce a central constant-density core. This phenomenon is called cusp-core problem. When dark matter is quiescent and satisfies the condition for hydrostatic equilibrium, using the equation of state can get the density profile in the static and spherically symmetric space-time. To solve the cusp-core problem, we assume that the equation of state is independent of the scaling transformation. Its lower order approximation for this type of equation of state can naturally lead to a special case, i.e. $p=ζρ+2εV_{rot}^{2}ρ$, where $p$ and $ρ$ are the pressure and density, $V_{rot}$ is the rotation velocity of galaxy, $ζ$ and $ ε$ are positive constants. It can obtain a density profile that is similar to the pseudo-isothermal halo model when $ε$ is around $0.15$. To get a more widely used model, let the equation of state include the polytropic model, i.e. $p= \fracζ{ρ_{0}^{s}}ρ^{1+s}+ 2εV_{rot}^{2}ρ$, we can get other kinds of density profiles, such as the profile that is nearly same with the Burkert profile, where $s$ and $ρ_{0}$ are positive constants.
