An Examination of Collisional Growth of Silicate Dust in Protoplanetary Disks
An Examination of Collisional Growth of Silicate Dust in Protoplanetary Disks
复制标题
原行星盘中硅酸盐尘埃碰撞生长的检验
DOI：
10.1088/2041-8205/783/2/l36
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
K.
中科院分区：
文献类型：
--
作者：
Yamamoto;T.; Kadono,T. and Wada;K.
到目前为止，对原行星盘中尘埃聚集体碰撞的N体模拟显示，如果碰撞速度高于约10 m s − 1，硅酸盐聚集体会遭受灾难性的破坏，这比在盘中预期的要低得多。这主要是由于模拟中使用的石英的表面能低。我们发现一个简单的表面能和熔化温度之间的关系，包括那些天体物理学的兴趣，各种材料，并表明，在以前的模拟中使用的石英的表面能远低于目前的估计。这一结果可能提供了一种方法，摆脱了在雪线内以圆盘形式生长硅酸盐尘埃的困难。我们表明，硅酸盐尘埃可以逃避灾难性的破坏和增长，即使在高速碰撞预计在磁盘中，如果考虑到目前的估计表面能。
N-body simulations of collisions of dust aggregates in protoplanetary disks performed so far have revealed that silicate aggregates suffer from catastrophic disruption if the collision velocities are higher than about 10 m s− 1, which is much lower than those expected in the disks. This is mainly due to the low surface energy of the quartz used in the simulations. We find a simple relation between the surface energy and melting temperature for various materials including those of astrophysical interest, and show that the surface energy of the quartz used in the previous simulations is much lower than the present estimate. This result may provide a way out of the difficulty of growing silicate dust inside the snowline in disks. We show that silicate dust can evade catastrophic disruption and grow even at high-velocity collisions expected in the disks if one takes the present estimate of the surface energy into account.