复杂有机分子之旅：原始星云中形成与输运

复杂有机分子是分子多样性的指示器。它们在彗星、行星和卫星上的检测促使人们询问其来源，特别是有利于其形成的条件。一个假设认为，在原始日系气体盘中，对冰粒子的紫外线照射可产生显著的分子复杂性，该假设得到了甲醇冰照射实验的支持。我们研究了随着甲烷冰粒子在原始日系气体盘中的迁移而照射的过程。我们的目标是确定是否存在遇及的条件有助于形成复杂有机分子，我们在分析中利用了实验数据。我们 developed a two-dimensional model that describes the transport of pebbles during the evolution of the protosolar nebula, employing a Lagrangian scheme. This model computes the interstellar UV flux received by the particles along their paths, which we compared with experimental values. On average, particles ranging from 1 to 100 micrometers in size, released at a local temperature of 20 K, undergo adequate irradiation to attain the same molecular diversity as methanol ice during the experiments within timescales of 25 kyr of protosolar nebula evolution. In contrast, 1 cm sized particles require 911 kyr of irradiation to reach similar molecular diversity, making comparable molecular complexity unlikely. Similarly, particles ranging from 1 to 100 micrometers in size, released at a local temperature of 80 K, receive sufficient irradiation after 141 and 359 kyr. The particles readily receive the irradiation dose necessary to generate the molecular diversity observed in the experiments within the outer regions of the disk. Our model, combined with future irradiation experiments, can provide additional insights into the specific regions where the building blocks of planets form.