PAHs in circumstellar disks around Herbig Ae/Be stars
PAHs in circumstellar disks around Herbig Ae/Be stars
复制标题
Herbig Ae/Be 恒星周围星周盘中的 PAH
DOI：
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发表时间：
2004
期刊：
影响因子：
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通讯作者：
E. Krugel
中科院分区：
文献类型：
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作者：
É. Habart;A. Natta;E. Krugel
我们调查的存在和性质的多环芳烃的表面上的拱星盘周围Herbig Ae/Be星通过比较磁盘模型的预测与观测。我们目前的结果的辐射传输代码磁盘加热的中心星星，在流体静力平衡在垂直方向（耀斑磁盘）。尘埃是处于热平衡状态的大颗粒、瞬时加热的小颗粒和多环芳烃的混合物。特别关注恒星、盘面和多环芳烃性质对多环芳烃发射线强度及其空间分布的影响。这些模型预测了一个红外SED，在连续光谱上方3.3、6.2、7.7和11.3 µm处清晰可见的PAH特征，其中一些非常强烈。PAH发射，空间上扩展，主要来自外盘区域（R 100 Au），而在类似波长的连续发射，主要是由于温暖的大颗粒，被限制在最里面的磁盘区域（R几个Au）。我们比较模型的结果，从ISO和地面望远镜的红外观测的赫比格Ae/Be星的约30。大多数观测到的PAH功能的光谱类型晚于B 9的对象很好地描述了我们的磁盘模型，我们讨论了一些详细的PAH特性，可以从现有的数据。具有强辐射场的天体（通常早于B 9）具有3.3 µm的特征（通常是唯一观测到的特征），比预测的要弱得多，我们讨论了可能的解释（圆盘的耗散，光蒸发或PAH性质的修改）。
We investigate the presence and properties of PAHs on the surface of circumstellar disks around Herbig Ae/Be stars by comparing the predictions of disk models with observations. We present results of a radiation transfer code for disks heated by the central star, in hydrostatic equilibrium in the vertical direction (flared disks). The dust is a mixture of large grains in thermal equilibrium, transiently heated small grains and PAHs. Special attention is given to the influence of the stellar, disk and PAH properties on the strength of the PAH emission lines and their spatial distribution. The models predict an infrared SED showing PAH features at 3.3, 6.2, 7.7, and 11.3 µm clearly visible above the continuum, and with some of them very strong. The PAH emission, spatially extended, comes mostly from the outer disk region (R ∼ 100 AU) while the continuum emission at similar wavelengths, mostly due to warm large grains, is confined to the innermost disk regions (R ∼ few AU). We compare the model results to infrared observations from ISO and ground-based telescopes of some thirty Herbig Ae/Be stars. Most of the observed PAH features in objects with spectral type later than B9 are well described by our disk models and we discuss in some detail the PAH characteristics one can derive from the existing data. Objects with strong radiation field (generally earlier than about B9) have the 3.3 µm feature (often the only one observed) much weaker than predicted, and we discuss possible explanations (dissipation of the disk, photoevaporation or modification of the PAH properties).
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell