Equation of State for Neutralino Star as a Form of Cold Dark Matter

以便学习 neutralino 星和黑暗星系的结构，我们在 neutralino 事由于波色子交换考虑动态相互作用。与波色子考虑 neutralinos 的相互作用，我们以相对论的吝啬地的途径导出 neutralino 星的状态(曙光女神) 的方程。然后，我们使用产生曙光女神调查象它的密度侧面和集体限制那样的 neutralino 星的性质。例如，如果 neutralino 团在 1 TeV 附近， neutralino 星的奥本海默团限制作为 6.06 ×被获得 10 -7 M , 和相应半径是大约 7.8 公里。由于由我们的计算显示了的增加的歼灭率，这个稠密的状态永远不能实际上在实践被认识到。我们的结果也证明低密度的 neutralino 星可以是冷黑暗的事的可能的聚集。

In order to study the structure of neutralino star and dark galaxy, we consider dynamical interactions due to boson-exchange in the neutralino matter. Taking into account interactions of neutralinos with bosons, we derive the equation of state （EOS） of neutralino stars in terms of the relativistic mean-field approach. Then we apply the resulting EOS to investigate properties of the neutralino star such as its density profile and mass limit. For example, if the neutralino mass is around 1 TeV, the Oppenheimer mass limit of the neutralino star is obtained as 6.06 ×10^-7 M⊙, and the corresponding radius is about 7.8 mm. Actually, due to an increasing annihilation rate as indicated by our calculation, this dense state can never be realized in practice. Our results also show that the low-density neutralino star may be a possible aggregation of the cold dark matter.