太阳星云中热矿物的光泳输运
Photophoretic transport of hot minerals in the solar nebula
摘要：
在大量彗星中发现了高温矿物，并且在星尘任务返回的Wild 2彗星样本中也发现了高温矿物。与此同时，对年轻恒星系统中热矿物质分布的观测表明，这些物质产生于原始星云的内部，并在彗星形成区向外输送。我们调查的可能性，电泳提供了一个可行的机制，运输高温材料从内太阳系的彗星形成的地区。我们使用一个网格的时间依赖磁盘模型的太阳星云量化的距离范围内，热矿物可以从磁盘的内部向其外部区域作为其大小和密度的函数。这里考虑的粒子是以聚集体的形式存在的，它们可能是由热矿物单个颗粒聚集而成的，这些颗粒的尺寸可以小到亚微米级，并在太阳星云最热的部分凝结形成。我们的粒子输运模型包括电泳，辐射压力和气体阻力。根据假设的盘参数和粒子密度，10-2到10-1 m的聚集体可以在很短的时间尺度（不超过几十万年）内到达原始星云中的日心距离高达35 AU。10-3 m粒子遵循与较大粒子相同的轨迹，但它们的最大迁移距离不超过26 AU，并且在盘中较晚的时期达到。另一方面，在太阳星云的演化过程中，10-5到10-4 m的聚集体不断被向外推。我们的模拟表明，无论采用的太阳星云模型，电泳是一种机制，可以解释热温度矿物的彗星的形成区域的存在。
英文摘要：
Hot temperature minerals have been detected in a large number of comets and were also identified in the samples of Comet Wild 2 that were returned by the Stardust mission. Meanwhile, observations of the distribution of hot minerals in young stellar systems suggest that these materials were produced in the inner part of the primordial nebula and have been transported outward in the formation zone of comets. We investigate the possibility that photophoresis provides a viable mechanism to transport high-temperature materials from the inner solar system to the regions in which the comets were forming. We use a grid of time-dependent disk models of the solar nebula to quantify the distance range at which hot minerals can be transported from the inner part of the disk toward its outer regions as a function of their size and density. The particles considered here are in the form of aggregates that presumably were assembled from hot mineral individual grains ranging down to submicron sizes and formed by condensation within the hottest portion of the solar nebula. Our particle-transport model includes the photophoresis, radiation pressure, and gas drag. Depending on the postulated disk parameters and the density of particles, 10-2 to 10-1 m aggregates can reach heliocentric distances up to 35 AU in the primordial nebula over very short timescales (no more than a few hundred thousand years). 10-3 m particles follow the same trajectory as the larger ones but their maximum migration distance does not exceed 26 AU and is reached at later epochs in the disks. On the other hand, 10-5 to 10-4 m aggregates are continuously pushed outward during the evolution of the solar nebula. Our simulations suggest that irrespective of the employed solar nebula model, photophoresis is a mechanism that can explain the presence of hot temperature minerals in the formation region of comets.
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