The Physical and Chemical Structure of Hot Molecular Cores
The Physical and Chemical Structure of Hot Molecular Cores
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DOI：
10.1051/0004-6361:20031646
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发表时间：
2003-11
影响因子：
6.5
通讯作者：
H. Nomura;Thomas J. Millar
中科院分区：
文献类型：
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作者：
H. Nomura;Thomas J. Millar
我们使用详细的辐射传输模型以及对热分子核心光谱能量分布的观察，对嵌入发光物体周围的气体和尘埃的密度和温度分布进行了自洽模型。利用这些剖面，我们研究了颗粒地幔蒸发时产生的热核心化学反应，考虑到地幔分子的不同结合能，以及我们假设所有分子都嵌入水冰中并具有共同结合能的模型。我们发现，大多数所得的柱密度与中心发光恒星形成后 10 4 年左右时向热核心 G34.3+0.15 观察到的柱密度一致。我们还研究了化学结构对密度分布的依赖性，这表明通过确定解吸分子的线发射源尺寸来约束密度分布的观察可能性。
We have made self-consistent models of the density and temperature profiles of the gas and dust surrounding embedded luminous objects using a detailed radiative transfer model together with observations of the spectral energy distribution of hot molecular cores. Using these profiles we have investigated the hot core chemistry which results when grain mantles are evaporated, taking into account the different binding energies of the mantle molecules, as well a model in which we assume that all molecules are embedded in water ice and have a common binding energy. We find that most of the resulting column densities are consistent with those observed toward the hot core G34.3+0.15 at a time around 10 4 years after central luminous star formation. We have also investigated the dependence of the chemical structure on the density profile which suggests an observational possibility of constraining density profiles from determination of the source sizes of line emission from desorbed molecules.