Anatomy of the Photodissociation Region in the Orion Bar
Anatomy of the Photodissociation Region in the Orion Bar
复制标题
DOI：
10.1126/science.262.5130.86
复制
发表时间：
1993-10
期刊：
影响因子：
56.9
通讯作者：
A. Tielens;M. Meixner;P. P. van der Werf-P.;J. Bregman;J. Tauber;J. Stutzki;D. Rank
中科院分区：
文献类型：
--
作者：
A. Tielens;M. Meixner;P. P. van der Werf-P.;J. Bregman;J. Tauber;J. Stutzki;D. Rank
许多星际气体存在于光解离区域，其化学和能量平衡由其上的远紫外线辐射通量控制。这些光子可以电离和解离分子，并通过作用于尘埃颗粒的光电效应加热气体。这些区域已在理论上进行了广泛的建模，但详细的观察研究很少。在与多环芳烃的碳-氢伸缩模式、分子氢的 1-0 S(1) 线和一氧化碳的 J = 1-0 旋转线相对应的波长处绘制突出的 Orion Bar 光解离区域，可以追踪远紫外线辐射穿透到云中的情况。结果有力地支持了理论模型，并最终表明，入射远紫外辐射场，而不是有时提出的激波，是猎户座棒中发射的原因。
Much of the interstellar gas resides in photodissociation regions whose chemistry and energy balance is controlled by the flux of far-ultraviolet radiation upon them. These photons can ionize and dissociate molecules and heat the gas through the photoelectric effect working on dust grains. These regions have been extensively modeled theoretically, but detailed observational studies are few. Mapping of the prominent Orion Bar photodissociation region at wavelengths corresponding to the carbon-hydrogen stretching mode of polycyclic aromatic hydrocarbons, the 1-0 S(1) line of molecular hydrogen, and the J = 1-0 rotational line of carbon monoxide allows the penetration of the far-ultraviolet radiation into the cloud to be traced. The results strongly support the theoretical models and show conclusively that the incident far-ultraviolet radiation field, not shocks as has sometimes been proposed, is responsible for the emission in the Orion Bar.