Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores. I. Spectral energy distributions and evolutionary sequence
Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores. I. Spectral energy distributions and evolutionary sequence
复制标题
塌陷低质量致密岩心中第一个静水岩心的综合观测。
DOI：
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发表时间：
2012
期刊：
影响因子：
--
通讯作者：
T. Henning
中科院分区：
文献类型：
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作者：
B. Commerçon;R. Launhardt;C. Dullemond;T. Henning
上下文。从观测和理论考虑来看，低质量恒星形成的演化序列都是相对明确的。第一个流体静力核是在恒星形成过程中形成的第一个原恒星或平衡物体。目标。利用最先进的辐射磁流体力学三维自适应网格细化计算，我们的目标是为第一个流体静力岩心的粉尘连续发射提供p预测。方法。我们利用RAMSES代码研究了磁化1 M⊙星前致密核的坍缩和破碎，以及第一流体静力核的形成和演化。我们使用了三种不同的磁化水平作为初始条件，这涵盖了各种各样的早期进化形态，例如，圆盘或伪圆盘的形成，流出发射和破碎。我们使用三维辐射传输代码deradmc -3D对动力学计算进行后处理。我们计算了光谱能量分布和通常的进化阶段指标，如热光度和温度。结果。我们发现第一个流体静力核的寿命在很大程度上取决于母致密核的初始磁化水平。我们首次从高分辨率辐射磁流体动力学计算中推导出光谱能量分布演化序列。结果表明，在一定条件下，可以从24µm和70µm的粉尘连续体发射离子中识别出第一h静压岩心。我们还表明，单谱能量分布不能帮助区分第一个流体静力核的形成情景，即磁化和非磁化模型之间的区别。结论。光谱能量分布是确定第一个流体静力岩心候选者的第一个有用和直接的方法，但确定观察到的源的演化阶段肯定需要高分辨率干涉测量。
Context. The low-mass star formation evolutionary sequence is relatively well-defined both from observations and theoretical c onsiderations. The first hydrostatic core is the first protostella r equilibrium object that is formed during the star formation process. Aims. Using state-of-the-art radiation-magneto-hydrodynamic 3D adaptive mesh refinement calculations, we aim to provide p redictions for the dust continuum emission from first hydrostatic cores. Methods. We investigated the collapse and the fragmentation of magnetized 1 M⊙ prestellar dense cores and the formation and evolution of first hydrostatic cores using the RAMSES code. We used three different magnetization levels for the initial conditions, whi ch cover a wide variety of early evolutionary morphology, e.g., the formation of a disk or a pseudo-disk, outflow launching, and fragmentation. We post-processed the dynamical calculations using the 3D radiative transfer codeRADMC-3D. We computed spectral energy distributions and usual evolutionary stage indicators suc h as bolometric luminosity and temperature. Results. We find that the first hydrostatic core lifetimes depend stron gly on the initial magnetization level of the parent dense core. We derive, for the first time, spectral energy distribution evo lutionary sequences from high-resolution radiation-magneto-hydrodynamic calculations. We show that under certain conditions, first h ydrostatic cores can be identified from dust continuum emiss ion at 24 µm and 70 µm. We also show that single spectral energy distributions cannot help in distinguishing between the formation scenarios of the first hydrostatic core, i.e., between the magnetized and non-magnetized models. Conclusions. Spectral energy distributions are a first useful and direct w ay to target first hydrostatic core candidates but highresolution interferometry is definitively needed to determ ine the evolutionary stage of the observed sources.
DOI：
10.1088/0067-0049/188/1/139
发表时间：
2010-04
期刊：
The Astrophysical Journal Supplement Series
影响因子：
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作者：
R. Launhardt;D. Nutter;D. Ward-Thompson;T. Bourke;T. Henning;T. Khanzadyan;T. Khanzadyan;M. Schmalzl;S. Wolf;S. Wolf;R. Zylka
通讯作者：
R. Launhardt;D. Nutter;D. Ward-Thompson;T. Bourke;T. Henning;T. Khanzadyan;T. Khanzadyan;M. Schmalzl;S. Wolf;S. Wolf;R. Zylka