Planet formation - Mechanism of early growth
Planet formation - Mechanism of early growth
复制标题
行星形成 - 早期生长机制
DOI：
10.1016/0019-1035(78)90023-4
复制
发表时间：
1978
期刊：
影响因子：
3.2
通讯作者：
J. Bassler
中科院分区：
文献类型：
--
作者：
W. Meeks;J. Bassler
真空实验(约0.5到1mbar)，并在空气中量化低速(1-50m/秒)下的碰撞、反弹和碎裂的机制，在通常假设的原始太阳星云的行星前环境条件下。这样的碰撞在实验上很少被研究。与普遍的假设相反，在一个给定的群体中，最大的流星和小行星大小的天体的增长是由这些碰撞的简单机制自发产生的，而没有其他特别的粘连机制。蜂群中较小的身体不太可能生长。颗粒状表面的形成，要么是由于尘埃群的重力崩塌，要么是由于固体行星上风化层表面的快速形成；这些表面通过抑制反弹而有力地促进了进一步的增长。大型天体的增长增加了模式碰撞速度，导致较小天体的碎裂，并最终产生星际尘埃，作为行星-小行星相互作用的副产品。
Experiments in vacuum (approx. 0.5 to 1 mbar) and in air quantify mechanics of collisions, rebound, and fragmentation at low velocities (1–50 m/sec), under the conditions usually postulated for the preplanetary environment in the primitive solar nebula. Such collisions have been little studied experimentally. Contrary to widespread assumptions, accretionary growth of the largest meteoroid- and asteroid-sized bodies in a given swarm results spontaneously from the simple mechanics of these collisions, without other ad hoc sticking mechanisms. The smaller bodies in the swarm are less likely to grow. Granular surfaces form, either by gravitational collapse of dust swarms or by rapid formation of regolith surfaces on solid planetesimals; these surfaces strongly promote further growth by retarding rebound. Growth of large bodies increases modal collision velocities, causing fragmentation of smaller bodies and eventual production of interstellar dust as a by-product planetesimal interactions.