arXiv 0712.23332007-12-14astro-ph

大质量原恒星尘埃和分子辐射模型

Models for Dust and Molecular Emission of High-Mass Protostars

Mayra Osorio

备注：: 8 pages, 5 figures. Conference: "Massive Star Formation: Observations confront Theory" 2007, Heidelberg Germany. To appear in Astronomical Society of the Pacific

摘要：

我们提出了一个详细的建模的结果，旨在重现的光谱能量分布（SED）的尘埃和大规模的原恒星的分子线发射的假设下，他们通过吸积过程形成。我们模拟的排放起源于降落信封在尺度小于0.1 pc的中央原恒星。为此，我们将我们的模型结果与覆盖广泛波长的观测数据进行了比较，特别注意双子座天文台获得的高角分辨率中红外数据和VLA在厘米波长处观察到的氨线发射。我们探索了两种模型信封。在第一类模型中，假设球对称，并计算了降落包层的SED以及氨排放。通过这种方法，可以获得沿岩心的温度、密度、速度、速度弥散和氨丰度变化。第二种方法考虑了偏离球面对称的情况，并且可以通过SED拟合来约束诸如核心的旋转、伸长程度或系统的倾斜度等参数。使用这两种方法，我们已经能够模拟大质量恒星的形成，其细节程度与低质量恒星相似。

英文摘要：

We present the results of a detailed modeling aimed to reproduce the spectral energy distribution (SED) of dust and molecular line emission of massive protostars under the hypothesis that they form via an accretion process. We model the emission originated in the infalling envelopes at scales smaller than 0.1 pc from the central protostar. To do that, we compared our model results with observational data covering a wide range of wavelengths, paying special attention to the high angular resolution mid-infrared data obtained with the Gemini Observatory and the ammonia line emission observed with the VLA at centimeter wavelengths. We have explored two kind of model envelopes. In the first kind of models, spherical symmetry is assumed and the SED as well as the ammonia emission of the infalling envelope are calculated. In this way, the temperature, density, velocity, velocity dispersion, and ammonia abundance variations along the core can be obtained. The second approach takes into account deviations from the spherical symmetry, and parameters such as the rotation, degree of elongation of the core, or inclination of the system can be constrained through the SED fitting. Using these two approaches we have been able to model the formation of massive stars with a degree of detail similar to that reached for the low mass stars.

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