灾难性小天体碰撞的全数值模拟
Full Numerical Simulations of Catastrophic Small Body Collisions
摘要：
小型冰体（如柯伊伯带天体）之间碰撞的结果知之甚少，但却是外海王星区域演化的关键组成部分。外太阳系物质的预期物理性质（高孔隙度，混合冰岩成分和低材料强度）构成了重大的计算挑战。我们目前的结果从灾难性的小天体碰撞使用一个新的混合水代码$N$体代码计算技术。该方法允许对冲击波传播和材料改性以及重力再积累进行详细建模。在这里，我们考虑了广泛的材料强度，以跨越柯伊伯带天体的可能范围。我们发现，剪切强度的目标是重要的，在确定碰撞结果为2至50公里半径的机构，这是传统上被认为是在一个纯重力制度。灾难性破裂和分散标准$Q_D^*$在强结晶和弱聚集材料之间可以变化高达三倍。在最大的再积累残留物中的物质经历了大范围的冲击压力。分散和重新积聚的过程导致最大残留物表面的物质与内部物质相比经历了更大范围的冲击压力。因此，取决于初始结构和组成，外太阳系中大型再积累天体的表面物质可能会表现出复杂的光谱和日冕变化。最后，我们提出了一系列的影响速度和材料强度外太阳系天体的修订灾难性破坏标准。
英文摘要：
The outcome of collisions between small icy bodies, such as Kuiper belt objects, is poorly understood and yet a critical component of the evolution of the trans-Neptunian region. The expected physical properties of outer solar system materials (high porosity, mixed ice-rock composition, and low material strength) pose significant computational challenges. We present results from catastrophic small body collisions using a new hybrid hydrocode to $N$-body code computational technique. This method allows detailed modeling of shock propagation and material modification as well as gravitational reaccumulation. Here, we consider a wide range of material strengths to span the possible range of Kuiper belt objects. We find that the shear strength of the target is important in determining the collision outcome for 2 to 50-km radius bodies, which are traditionally thought to be in a pure gravity regime. The catastrophic disruption and dispersal criteria, $Q_D^*$, can vary by up to a factor of three between strong crystalline and weak aggregate materials. The material within the largest reaccumulated remnants experiences a wide range of shock pressures. The dispersal and reaccumulation process results in the material on the surfaces of the largest remnants having experienced a wider range of shock pressures compared to material in the interior. Hence, depending on the initial structure and composition, the surface materials on large, reaccumulated bodies in the outer solar system may exhibit complex spectral and albedo variations. Finally, we present revised catastrophic disruption criteria for a range of impact velocities and material strengths for outer solar system bodies.
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