Physical parameters for Orion KL from modelling its ISO high-resolution far-IR CO line spectrum
Physical parameters for Orion KL from modelling its ISO high-resolution far-IR CO line spectrum
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Orion KL 的物理参数，来自对其 ISO 高分辨率远红外 CO 线谱建模
DOI：
10.1111/j.1365-2966.2008.13349.x
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发表时间：
2008
影响因子：
4.8
通讯作者：
Lerate M
中科院分区：
文献类型：
--
作者：
Lerate M
作为猎户座Kleinmann-Low（KL）区域的第一次高分辨率远红外（far-IR）光谱调查的一部分，我们观察到20条CO发射线，Jup = 16至39（基态以上从752至4294 K的上能级）。观测是使用红外空间观测站（ISO）上的长波分光仪以其高分辨率法布里-珀罗（FP）模式（每秒33公里）进行的。我们在这里提出了一个分析的最终校准CO数据，执行一个更复杂的建模技术比迄今为止，包括化学的详细分析，并讨论与以前的结果的相似性和差异。包括化学建模意味着原子和分子丰度是由化学预测的时间。这提供了一个主要的区别与以往的研究中，化学丰度需要假设为初始条件。通过模拟KL区域不同已知成分的条件来研究该区域的化学：热核、高原和脊的化学模型与加速Λ迭代（ALI）辐射传输模型相结合，以预测线通量和剖面。我们的结论是，18 <Jup< 25的CO跃迁主要来自直径为0.02 pc、密度为107 cm − 3的热核，而不是像以前的研究所指出的那样来自平台。其余的跃迁来自于直径为10.06 pc，密度为3 × 105 ~ 1 × 106 cm −3的激波气体。由此得到的CO丰度分数在X（CO）=（7.0-4.7）× 10−5的范围内。达到Jup> 32的转变需要一个大于1000 K的高温激波后区，而Jup < 18的转变可能起源于扩展的暖分量。最后，我们讨论了空间起源的CO排放相比，下一个最丰富的物种检测到的远红外调查猎户座KL：H2O和OH。
As part of the first high-resolution far-infrared (far-IR) spectral survey of the Orion Kleinmann–Low (KL) region, we observed 20 CO emission lines withJup= 16 to 39 (upper levels from ≈752 to 4294 K above the ground state). Observations were taken using the Long Wavelength Spectrometer on board theInfrared Space Observatory(ISO), in its high-resolution Fabry–Pérot (FP) mode (≈33 km s−1). We present here an analysis of the final calibrated CO data, performed with a more sophisticated modelling technique than hitherto, including a detailed analysis of the chemistry, and discuss similarities and differences with previous results. The inclusion of chemical modelling implies that atomic and molecular abundances are time predicted by the chemistry. This provides one of the main differences with previous studies in which chemical abundances needed to be assumed as initial condition. The chemistry of the region is studied by simulating the conditions of the different known components of the KL region: chemical models for a hot core, a plateau and a ridge are coupled with an accelerated Λ-iteration (ALI) radiative transfer model to predict line fluxes and profiles. We conclude that the CO transitions with 18 <Jup< 25 mainly arise from a hot core of diameter 0.02 pc and a density of 107cm−3rather from the plateau as previous studies had indicated. The rest of the transitions originate from shocked gas in a region of diameter ≈0.06 pc with densities ranging from 3 × 105to 1 × 106cm−3. The resulting CO fractional abundances are in the rangeX(CO) = (7.0–4.7) × 10−5. A high-temperature post-shock region at more than 1000 K is necessary to reach transitions withJup> 32, whilst transitions withJup< 18 probably originate from the extended warm component. Finally, we discuss the spatial origin of the CO emission compared with that of the next most abundant species detected by the far-IR survey towards Orion KL: H2O and OH.
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发表时间：
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