灶神星的加热历史和分异的开始
The heating history of Vesta and the onset of differentiation
摘要：
在这项工作中，我们研究了灶神星的内部结构的演变和热加热之间的联系，由于26铝和60铁和长寿命的放射性核素，考虑到身体的化学分化和26铝与硅酸盐的亲和力。分化发生在所有的情况下，在灶神星完成其吸积在不到1.4 Ma后注入26铝到太阳星云。在所有这些情况下，灶神星在不到1 Ma的时间内从26 Al注入完成其形成，整个小行星的硅酸盐熔化程度达到100体积%。如果灶神星在注入26铝后的1 ~ 1.4 Ma之间完成了它的形成，那么硅酸盐熔融的程度在整个小行星上超过50体积%，但在所有孔隙度低于5体积%的情况下，只有在地幔最热的最外层部分才达到100体积%。如果灶神星的形成发生在注入26 Al之后的1.5 Ma之后，硅酸盐熔融的程度总是低于50体积%，并且仅限于小行星的一小部分区域。5 Ma后，地壳厚度从8 ~ 30 km不等，其中约3-20 km为原始未熔融的铁电质，约5-10 km为真晶质。
英文摘要：
In this work we study the link between the evolution of the internal structure of Vesta and thermal heating due to 26Al and 60Fe and long-lived radionuclides, taking into account the chemical differentiation of the body and the affinity of 26Al with silicates. Differentiation takes place in all scenarios in which Vesta completes its accretion in less than 1.4 Ma after the injection of 26Al into the Solar Nebula. In all those scenarios where Vesta completes its formation in less than 1 Ma from the injection of 26Al, the degree of silicate melting reaches 100 vol. % throughout the whole asteroid. If Vesta completed its formation between 1 and 1.4 Ma after 26Al injection, the degree of silicate melting exceeds 50 vol. % over the whole asteroid but reaches 100 vol. % only in the hottest, outermost part of the mantle in all scenarios where the porosity is lower than 5 vol. %. If the formation of Vesta occurred later than 1.5 Ma after the injection of 26Al, the degree of silicate melting is always lower than 50 vol. % and is limited only to a small region of the asteroid. The radiation at the surface dominates the evolution of the crust which ranges in thickness from 8 to about 30 km after 5 Ma: a layer about 3-20 km thick is composed of primitive unmelted chondritic material while a layer of about 5-10 km is eucritic.
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