Following the Interstellar History of Carbon: From the Interiors of Stars to the Surfaces of Planets
Following the Interstellar History of Carbon: From the Interiors of Stars to the Surfaces of Planets
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追踪碳的星际历史：从恒星内部到行星表面
DOI：
10.1089/ast.2016.1484
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发表时间：
2016
期刊：
影响因子：
4.2
通讯作者：
Y
中科院分区：
文献类型：
--
作者：
Ziurys;L. M.;Halfen;D. T.;Geppert;W.;Aikawa;Y
碳的化学历史可以追溯到它在恒星核合成中的起源，直到它被运送到行星表面。这种元素的分子载体在星际有机物循环的每个阶段以及它们最终并入太阳系天体的过程中都要进行检查。还研究了各种星际碳储层之间的联系。碳有两种恒星来源：超新星爆炸和演化恒星的质量损失。在后一种情况下，碳从内部被挖掘出来，然后喷射到星周包层中，在那里发生了丰富而不寻常的c基化学反应。这些分子物质最终通过行星状星云释放到一般的星际介质中。它首先被纳入漫射云中，在云中，碳以多原子分子的形式存在，如H2CO、HCN、HNC、c-C3H2，甚至C60+。然后这些物体坍缩成稠密的云，恒星和行星形成的地方。这样的云形成了一种活跃的有机化学，产生了具有气相和表面机制的多种官能团的化合物。随着恒星和行星的形成，恒星辐射的增加以及太阳系前星云的反应可能会改变化学成分。然而，一些富含碳的分子物质仍然是原始的，它们被包裹在彗星、陨石和行星际尘埃颗粒中，并被运送到行星表面。关键词：碳同位素-益生元演化-星际分子-彗星-陨石天体生物学16,997-1012。
The chemical history of carbon is traced from its origin in stellar nucleosynthesis to its delivery to planet surfaces. The molecular carriers of this element are examined at each stage in the cycling of interstellar organic material and their eventual incorporation into solar system bodies. The connection between the various interstellar carbon reservoirs is also examined. Carbon has two stellar sources: supernova explosions and mass loss from evolved stars. In the latter case, the carbon is dredged up from the interior and then ejected into a circumstellar envelope, where a rich and unusual C-based chemistry occurs. This molecular material is eventually released into the general interstellar medium through planetary nebulae. It is first incorporated into diffuse clouds, where carbon is found in polyatomic molecules such as H2CO, HCN, HNC,c-C3H2, and even C60+. These objects then collapse into dense clouds, the sites of star and planet formation. Such clouds foster an active organic chemistry, producing compounds with a wide range of functional groups with both gas-phase and surface mechanisms. As stars and planets form, the chemical composition is altered by increasing stellar radiation, as well as possibly by reactions in the presolar nebula. Some molecular, carbon-rich material remains pristine, however, encapsulated in comets, meteorites, and interplanetary dust particles, and is delivered to planet surfaces. Key Words: Carbon isotopes—Prebiotic evolution—Interstellar molecules—Comets—Meteorites. Astrobiology 16, 997–1012.