DISK MASSES AT THE END OF THE MAIN ACCRETION PHASE: CARMA OBSERVATIONS AND MULTI-WAVELENGTH MODELING OF CLASS I PROTOSTARS
DISK MASSES AT THE END OF THE MAIN ACCRETION PHASE: CARMA OBSERVATIONS AND MULTI-WAVELENGTH MODELING OF CLASS I PROTOSTARS
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主吸积阶段结束时的盘质量：I 类原恒星的 Carma 观测和多波长建模
DOI：
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发表时间：
2012
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通讯作者：
J. Eisner
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作者：
J. Eisner
我们展示了用 CARMA 干涉仪获得的金牛座恒星形成区 I 类原恒星 1.3 毫米波长的成像观测结果。在 10 个物体的初始样本中，我们检测到了 9 个物体的毫米波长发射并对其进行了成像。这 9 个物体中的一个被分解为两个源，对该二元原恒星系统的详细分析将推迟到未来的论文中。对于其余八个物体，我们使用 CARMA 数据来确定毫米发射的基本形态。将毫米级数据与 0.9μm 散射光图像、斯皮策红外光谱仪光谱和宽带光谱能量分布（全部来自文献）相结合，我们尝试确定星周物质的结构。我们考虑的模型包括星周盘和包层，并约束每个组件的质量（和其他结构参数）。我们表明样本中的圆盘质量范围从 ≲ 0.01 到 ≳ 0.1 M☉。我们的样本的圆盘质量明显高于更进化的 II 类天体样本。因此，I 类盘质量可能为恒星和行星形成的初始质量预算提供更准确的估计。然而，这里确定的盘质量低于巨行星形成理论所需的质量。对于重力不稳定而言，质量也显得太低，这可能导致较高的质量吸积率。即使在这些 I 类盘中，大量的粒子生长也可能将大部分盘质量隐藏在难以看到的较大物体中。
We present imaging observations at the 1.3 mm wavelength of Class I protostars in the Taurus star-forming region, obtained with the CARMA interferometer. Of an initial sample of 10 objects, we detected and imaged millimeter wavelength emission from 9. One of the nine is resolved into two sources and detailed analysis of this binary protostellar system is deferred to a future paper. For the remaining eight objects, we use the CARMA data to determine the basic morphology of the millimeter emission. Combining the millimeter data with 0.9 μm images of scattered light, Spitzer Infrared Spectrograph spectra, and broadband spectral energy distributions (all from the literature), we attempt to determine the structure of the circumstellar material. We consider models including both circumstellar disks and envelopes, and constrain the masses (and other structural parameters) of each of these components. We show that the disk masses in our sample span a range from ≲ 0.01 to ≳ 0.1 M☉. The disk masses for our sample are significantly higher than for samples of more evolved Class II objects. Thus, Class I disk masses probably provide a more accurate estimate of the initial mass budget for star and planet formation. However, the disk masses determined here are lower than required by theories of giant planet formation. The masses also appear too low for gravitational instability, which could lead to high mass accretion rates. Even in these Class I disks, substantial particle growth may have hidden much of the disk mass in hard-to-see larger bodies.