arXiv 1002.18642010-02astro-ph.GA

应用于大质量恒星的恒星形成标准模型：分子线中的吸积盘和包层

The standard model of star formation applied to massive stars: accretion disks and envelopes in molecular lines

Eric Keto, Qizhou Zhang

备注：: Accepted MNRAS
DOI：: 10.1111/j.1365-2966.2010.16672.x

摘要：

我们通过新的分子线观测和大质量原恒星IRAS 20126 +4104周围吸积流的建模来解决高质量恒星的形成是否与太阳质量恒星的形成相似或不同的问题。我们结合了在甚大阵列上对NH3（1，1）和（2，2）的新观测，在亚毫米阵列上对CHCN（13-12）的新观测，以前对NH（3，3），NH（4，4）的VLA观测，以及以前对C34 S（2-1），C34 S（5-4），和CHCN（12-11），以获得激发能覆盖15至419 K的分子谱线的数据集。我们比较这些观测结果与模拟分子线光谱预测的模型为高质量的恒星形成的基础上，按比例放大版本的标准盘信封范例周围的低质量恒星的吸积流。我们发现，在符合标准的范例，观测需要一个温暖的，密集的，快速旋转的磁盘和一个冷的，弥漫的下降信封。这项研究表明，10 M恒星周围的吸积过程类似于太阳质量的恒星。

英文摘要：

We address the question of whether the formation of high-mass stars is similar to or differs from that of solar-mass stars through new molecular line observations and modeling of the accretion flow around the massive protostar IRAS20126+4104. We combine new observations of NH3(1,1) and (2,2) made at the Very Large Array, new observations of CHCN(13-12) made at the Submillimeter Array, previous VLA observations of NH(3,3), NH(4,4), and previous Plateau de Bure observations of C34S(2-1), C34S(5-4), and CHCN(12-11) to obtain a data set of molecular lines covering 15 to 419 K in excitation energy. We compare these observations against simulated molecular line spectra predicted from a model for high-mass star formation based on a scaled-up version of the standard disk-envelope paradigm developed for accretion flows around low-mass stars. We find that in accord with the standard paradigm, the observations require both a warm, dense, rapidly-rotating disk and a cold, diffuse infalling envelope. This study suggests that accretion processes around 10 M stars are similar to those of solar mass stars.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

摘要：

英文摘要：

相关论文