Chemistry in Protoplanetary Disks

被引：196

作者：

Henning, Thomas ^{[1
]}

Semenov, Dmitry ^{[1
]}

机构：

[1] Max Planck Inst Astron, D-69117 Heidelberg, Germany

来源：

CHEMICAL REVIEWS | 2013年 / 113卷 / 12期

关键词：

POLYCYCLIC AROMATIC-HYDROCARBONS; MOLECULAR-HYDROGEN EMISSION; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DUST DISKS; CARLO RADIATIVE-TRANSFER; LOW-MASS PROTOSTELLAR; SIZED CARBON GRAINS; HERBIG AE/BE STARS; X-RAY IONIZATION;

D O I：

10.1021/cr400128p

中图分类号：

O6 [化学];

学科分类号：

0703 ;

摘要：

The wide range of planetary system architectures and exoplanet properties is certainly linked to a range of properties of their birth-places, the disk-like structures around young stars composed of gas and dust particles. These disks share many of the properties of the solar nebula from which the Sun and our planetary system formed, although their masses, radial dimensions, and internal structures can be very different. Dust spectroscopy has revealed the mineralogical composition of the protoplanetary dust particles that are mostly found in the form of amorphous silicates, crystalline forsterite, water ice, and other molecular ices. There is strong observational evidence that the dust particles in disks can grow in size far beyond the typical sub-micrometer sizes of interstellar dust grains.

引用

页码：9016 / 9042

页数：27

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