暗物质耗散自相互作用后太阳周围的致密晕
Compact Halo around the Sun Accreted after Dark Matter Dissipative Self Interaction
摘要：
如果暗物质粒子由于其耗散的自散射而减速，除了在星系尺度上下沉以加速结构形成外，它还可以吸积到太阳等局部天体上，形成致密的晕。在一些简化的假设下，我们建立了基于椭圆轨道配分函数的Boltzmann方程组，并数值求解了吸积过程。我们发现轨道运行的暗物质粒子将在太阳周围形成一个晕，其密度分布在很宽的半径范围内与$r^{-1.6}$成正比。在地球周围，这种局部晕的贡献总是比银河系分量低几个数量级，而在以太阳为中心的一个很小的区域内，下沉的暗物质粒子可以导致比背景银河系分量大几个数量级的晕密度，特别是在小减速速度和大截面的参数区域内，这仍然符合当前的限制。这种潜在的暗物质局部晕具有显著的增强密度，如果存在相应的通道，将是一个非常有趣的暗物质间接探测源，作为例子，我们详细讨论了太阳方向γ射线谱的可能性。
英文摘要：
If dark matter particle can be decelerated due to its dissipative self scattering, except for sinking at the galaxy scale to speed up structure formation, it can also be accreted onto local celestial bodies such as the Sun, forming a compact halo. With some simplified assumptions we develop the Boltzmann equation set based on the partition function of the elliptical orbits, and numerically solve it for the accretion process. We find that the orbited dark matter particles will form a halo around the Sun, with the density profile well fitted to be proportional to $r^{-1.6}$ in a wide range of radius. While around the earth such local halo contribution is always several orders below the galactic component, in a very small region centered around the Sun the sunk dark matter particles can lead to a halo density several orders larger than the background galactic component, in particular in the parameter region of small deceleration speed and large cross section, which is still consistent with current constraints. Such potential dark matter local halo with significantly enhanced density will be a very interesting source for dark matter indirect detection if the corresponding channel exists, we discuss the possibility of the gamma-ray spectrum in the solar direction in some detail as an example.
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