论文标题
固体的热处理遇到年轻的Jovian核心
Thermal Processing of Solids Encountering a Young Jovian Core
论文作者
论文摘要
与太阳相比，木星相对于氢的增强已被解释为证据，表明其早期形成发生在n $ _ {2} $雪地（$ \ sim $ 20-40 au）之外。但是，在太阳星云耗散之前形成木星所需的快速增长将导致形成的行星的核心达到非常高的温度（$> $ 1000 K），这将导致其温暖周围的环境。在这里，我们探讨了发光的行星芯对最终积聚的固体的影响。我们发现，发生临界过渡发生，在积聚之前非常热（快速积聚）的核心驱动挥发物，而凉爽的核心（缓慢积聚）能够继承富含挥发性的富含富含挥发性的固体。考虑到木星的氮富集，如果它以n $ _ {2} $雪线形成，则其核心无法以10 $^{ - 10} $ M $ _ {\ odot} $ yr $ yr $^$^{ - 1} $以上的速率增添固体。我们的结果表明，在太阳星云的远端区域形成的木星要么是通过将其掺入更多的难治性载体中抑制了氮的损失，要么是因为它被困在较高温度下散发出的冰中。
Jupiter's enhancement in nitrogen relative to hydrogen when compared to the Sun has been interpreted as evidence that its early formation occurred beyond the N$_{2}$ snowline ($\sim$ 20-40 AU). However, the rapid growth necessary to form Jupiter before the dissipation of the solar nebula would lead to the forming planet's core reaching very high temperatures ($>$1000 K), which would lead to it warming its surroundings. Here, we explore the effects of a luminous planetary core on the solids that it ultimately accretes. We find that a critical transition occurs where very hot (rapidly accreting) cores drive off volatiles prior to accretion, while cool cores (slowly accreting) are able to inherit volatile rich solids. Given Jupiter's nitrogen enrichment, if it formed beyond the N$_{2}$ snowline, its core could not have accreted solids at a rate above 10$^{-10}$ M$_{\odot}$ yr$^{-1}$. Our results suggest that either Jupiter formed in more distal regions of the solar nebula, or nitrogen loss was suppressed, either by its incorporation in more refractory carriers or because it was trapped within ices which devolatilized at higher temperatures.
