标题： 基于详细颗粒物理学的不透明度揭示木星的形成 显示英文标题

标题： Formation of Jupiter using opacities based on detailed grain physics

摘要： 基于核心增生模型的数值模拟展示了在3个具有不同固体颗粒表面密度假设值的原始盘中，木星在5.2天文单位处的形成过程。行星胚胎包层中的尘埃 opacity 使用一个详细的模型计算得出，该模型包括尘埃沉降和凝聚，并且在每个时间和空间点重新计算了尘埃大小分布。 我们通常发现的opacity比之前计算中使用的星际介质值的2%要低[Hubickyj, O., Bodenheimer, P., Lissauer, J. J., 2005. Icarus 179, 415--431; Lissauer, J. J., Hubickyj, O., D'Angelo, G., Bodenheimer, P., 2009. Icarus 199, 338-350]。这些较低的opacity导致行星胚胎包层更快地散热和收缩。 对于给定的固体表面密度，新的计算结果显示相比于之前的计算，形成时间大幅缩短。形成时间被计算为1.0、1.9和4.0百万年，而固体核心质量分别为16.8、8.9和4.7个地球质量，对应的固体表面密度sigma分别为10、6和4克每平方厘米。对于sigma=10和sigma=6克每平方厘米，相比于使用旧的opacity近似方法的先前发表的计算，这些形成时间分别减少了超过50%和超过80%。 显示英文摘要

摘要： Numerical simulations, based on the core-nucleated accretion model, are presented for the formation of Jupiter at 5.2 AU in 3 primordial disks with three different assumed values of the surface density of solid particles. The grain opacities in the envelope of the protoplanet are computed using a detailed model that includes settling and coagulation of grains and that incorporates a recalculation of the grain size distribution at each point in time and space. We generally find lower opacities than the 2% of interstellar values used in previous calculations [Hubickyj, O., Bodenheimer, P., Lissauer, J. J., 2005. Icarus 179, 415--431; Lissauer, J. J., Hubickyj, O., D'Angelo, G., Bodenheimer, P., 2009. Icarus 199, 338-350]. These lower opacities result in more rapid heat loss from and more rapid contraction of the protoplanetary envelope. For a given surface density of solids, the new calculations result in a substantial speedup in formation time as compared with those previous calculations. Formation times are calculated to be 1.0, 1.9, and 4.0 Myr, and solid core masses are found to be 16.8, 8.9, and 4.7 Earth masses, for solid surface densities, sigma, of 10, 6, and 4 grams per squared centimeter, respectively. For sigma=10 and sigma=6 g/cm^2, respectively, these formation times are reduced by more than 50% and more than 80% compared with those in a previously published calculation with the old approximation to the opacity.