再论木星共振诱发的球粒形成
Revisiting Jovian-Resonance Induced Chondrule Formation
摘要：
有人提出，由木星平均运动共振扰动的星子是形成陨石球粒的冲击波的来源。据认为，这种冲击诱导球粒的形成需要星子相对于气体盘的速度在1天文单位的数量级> 7公里/秒。在以往的星子激发研究中，研究了木星平均运动共振和气体阻力的影响，但在小行星带中获得的速度最多为8 km/s，这不足以解释球粒的普遍存在。在本文中，我们重新检查木星共振的影响，并考虑到长期共振的小行星带所造成的气体盘的重力。我们发现，相对于气体盘的体积为几百公里的星子的速度超过12公里/秒，这是在3：1平均运动共振附近实现的。加热区域被限制在1.5 AU和3.5 AU之间的相对窄的带。我们的研究结果表明，陨石球粒有效地产生后，木星形成的小行星区域。我们还发现，许多微行星分散在海王星之外。我们的发现可以解释彗星中结晶硅酸盐的存在，如果分散的星子包括冲击加热处理的硅酸盐尘埃。
英文摘要：
It is proposed that planetesimals perturbed by Jovian mean-motion resonances are the source of shock waves that form chondrules. It is considered that this shock-induced chondrule formation requires the velocity of the planetesimal relative to the gas disk to be on the order of > 7 km/s at 1 AU. In previous studies on planetesimal excitation, the effects of Jovian mean-motion resonance together with the gas drag were investigated, but the velocities obtained were at most 8 km/s in the asteroid belt, which is insufficient to account for the ubiquitous existence of chondrules. In this paper, we reexamine the effect of Jovian resonances and take into account the secular resonance in the asteroid belt caused by the gravity of the gas disk. We find that the velocities relative to the gas disk of planetesimals a few hundred kilometers in size exceed 12 km/s, and that this is achieved around the 3:1 mean-motion resonance. The heating region is restricted to a relatively narrow band between 1.5 AU and 3.5 AU. Our results suggest that chondrules were produced effectively in the asteroid region after Jovian formation. We also find that many planetesimals are scattered far beyond Neptune. Our findings can explain the presence of crystalline silicate in comets if the scattered planetesimals include silicate dust processed by shock heating.
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