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arXiv 1207.0656astro-ph.SR
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坍塌的低质量致密岩心中第一个流体静力学岩心的综合观测。I.光谱能量分布与演化序列

Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores. I. Spectral energy distributions and evolutionary sequence

Benoit Commercon, Ralf Launhardt, Cornelis P. Dullemond, Thomas Henning

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accepted for publication in Astronomy and Astrophysics, 13 pages, 9 figures few langage corrections + change in the discussion
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摘要：

低质量恒星形成演化序列从观测和理论考虑都是相对明确的。第一个流体静力核心是第一个在恒星形成过程中形成的原恒星平衡天体。使用国家的最先进的辐射磁流体动力学三维自适应网格细化计算，我们的目标是提供预测的尘埃连续排放的第一流体静力学核心。我们用RAMSES程序研究了磁化的一个太阳质量的星前致密核的坍缩和碎裂以及第一流体静力核的形成和演化。我们使用三种不同的磁化水平的初始条件，其中涵盖了大量的早期进化形态，例如，盘或伪盘的形成、外流发射和碎裂。我们使用三维辐射转移程序RADMC-3D对动力学计算进行后处理。我们计算光谱能量分布和通常的进化阶段指标，如热光度和温度。我们发现，第一流体静力学核心的寿命强烈依赖于初始磁化水平的父致密的核心。我们推导出，第一次，光谱能量分布演化序列从高分辨率辐射磁流体动力学计算。我们表明，在一定条件下，第一流体静力学核心可以确定从尘埃连续排放在24微米和70微米。我们还表明，单谱能量分布不能帮助区分第一流体静力学核心的形成情景，即，磁化模型和非磁化模型之间的差异光谱能量分布是第一个有用的和直接的方式来瞄准第一个流体静力学核心候选人，但高分辨率的干涉测量是绝对需要的，以确定所观察到的源的演变阶段。

英文摘要：

The low-mass star formation evolutionary sequence is relatively well-defined both from observations and theoretical considerations. The first hydrostatic core is the first protostellar equilibrium object that is formed during the star formation process. Using state-of-the-art radiation-magneto-hydrodynamic 3D adaptive mesh refinement calculations, we aim to provide predictions for the dust continuum emission from first hydrostatic cores. We investigate the collapse and the fragmentation of magnetized one solar mass prestellar dense cores and the formation and evolution of first hydrostatic cores using the RAMSES code. We use three different magnetization levels for the initial conditions, which cover a large variety of early evolutionary morphology, e.g., the formation of a disk or a pseudo-disk, outflow launching, and fragmentation. We post-process the dynamical calculations using the 3D radiative transfer code RADMC-3D. We compute spectral energy distributions and usual evolutionary stage indicators such as bolometric luminosity and temperature. We find that the first hydrostatic core lifetimes depend strongly on the initial magnetization level of the parent dense core. We derive, for the first time, spectral energy distribution evolutionary sequences from high-resolution radiation-magneto-hydrodynamic calculations. We show that under certain conditions, first hydrostatic cores can be identified from dust continuum emission at 24 microns and 70 microns. We also show that single spectral energy distributions cannot help to distinguish between the formation scenarios of the first hydrostatic core, i.e., between the magnetized and non-magnetized models. Spectral energy distributions are a first useful and direct way to target first hydrostatic core candidates but high-resolution interferometry is definitively needed to determine the evolutionary stage of the observed sources.

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