Radio continuum observations of Class I protostellar discs in Taurus: constraining the greybody tail at centimetre wavelengths★
Radio continuum observations of Class I protostellar discs in Taurus: constraining the greybody tail at centimetre wavelengths★
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金牛座I类原恒星盘的射电连续谱观测：将灰体尾限制在厘米波长★
DOI：
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发表时间：
2011
期刊：
影响因子：
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通讯作者：
E. Waldram
中科院分区：
文献类型：
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作者：
A. Scaife;J. Buckle;R. Ainsworth;M. Davies;T. Franzen;K. Grainge;M. Hobson;N. Hurley;A. Lasenby;M. Olamaie;Y. Perrott;G. Pooley;T. Ray;J. Richer;C. Rodrı́guez;R. Saunders;M. Schammel;P. Scott;T. Shimwell;D. Titterington;E. Waldram
我们提出了深1.8厘米（16 GHz）的无线电连续成像的金牛座分子云中的7个年轻的恒星物体。这些物体以前已经在亚毫米到近红外范围内进行了广泛的研究，并对其光谱能量分布进行了建模，以提供可靠的物理和几何参数。我们使用这些新的数据来约束灰体光谱的长波长尾部的属性，预计这将主要由原恒星盘中的大尘埃颗粒的发射。我们发现光谱与预期这样的人口的不透明度指数一致，平均不透明度指数β = 0.26 +/- 0.22，表明光盘内的晶粒生长。我们使用光谱拟合联合无线电和submm数据分离的贡献，热尘埃和无线电发射在1.8厘米，并直接从厘米波尘埃的贡献获得光盘质量。我们发现，来自这些流量密度的假设下与文献一致的光盘质量系统高于那些从submm数据计算，并满足巨行星形成的标准在一些情况下。
We present deep 1.8 cm (16 GHz) radio continuum imaging of seven young stellar objects in the Taurus molecular cloud. These objects have previously been extensively studied in the submm to near-infrared range and their spectral energy distributions modelled to provide reliable physical and geometrical parameters. We use these new data to constrain the properties of the long-wavelength tail of the greybody spectrum, which is expected to be dominated by emission from large dust grains in the protostellar disc. We find spectra consistent with the opacity indices expected for such a population, with an average opacity index of beta= 0.26 +/- 0.22 indicating grain growth within the discs. We use spectra fitted jointly to radio and submm data to separate the contributions from thermal dust and radio emission at 1.8 cm and derive disc masses directly from the cm-wave dust contribution. We find that disc masses derived from these flux densities under assumptions consistent with the literature are systematically higher than those calculated from submm data, and meet the criteria for giant planet formation in a number of cases.