GAS GAPS IN THE PROTOPLANETARY DISK AROUND THE YOUNG PROTOSTAR HL TAU
GAS GAPS IN THE PROTOPLANETARY DISK AROUND THE YOUNG PROTOSTAR HL TAU
复制标题
DOI：
10.3847/2041-8205/820/2/l25
复制
发表时间：
2016-03
期刊：
影响因子：
--
通讯作者：
Hsi-Wei Yen;H. Liu;P. Gu;N. Hirano;Chin-Fei Lee;E. Puspitaningrum;S. Takakuwa
中科院分区：
文献类型：
--
作者：
Hsi-Wei Yen;H. Liu;P. Gu;N. Hirano;Chin-Fei Lee;E. Puspitaningrum;S. Takakuwa
我们分析了阿塔卡马大型毫米/亚毫米阵列长基线活动获得的I-II类原恒星HL Tau的HCO+（1-0）数据。我们生成的HCO+图像立方体的角分辨率为100.″07（100 Au），并进行方位角平均的图像立方体，以提高信噪比和测量的径向轮廓的HCO+集成强度。在径向强度分布中确定了两个半径为28和69 Au的间隙和一个中心空腔。内部HCO+间隙与半径为32 Au的毫米连续带间隙一致。外HCO+间隙位于半径为69 Au的毫米连续亮环处，并与半径为64和74 Au的两毫米连续间隙重叠。相反，中心腔的存在可能是由于3 mm连续谱发射的高光学深度，而不是HCO+气体的耗尽。我们从其强度分布推导出HCO+柱密度分布。从柱密度分布，内部和外部的HCO+间隙的半高宽估计都是1.14 Au，并且它们的深度估计是1.24和1.50。这些结果与形成（亚）木星质量行星所打开的缺口的预期是一致的，同时对仅包含尘埃性质和粒度变化的理论模型进行了严格的限制。
We have analyzed the HCO+ (1–0) data of the Class I–II protostar, HL Tau, obtained from the Atacama Large Millimeter/submillimeter Array long baseline campaign. We generated the HCO+ image cube at an angular resolution of ∼0.″07 (∼10 au) and performed azimuthal averaging on the image cube to enhance the signal-to-noise ratio and measure the radial profile of the HCO+ integrated intensity. Two gaps at radii of ∼28 and ∼69 au and a central cavity are identified in the radial intensity profile. The inner HCO+ gap is coincident with the millimeter continuum gap at a radius of 32 au. The outer HCO+ gap is located at the millimeter continuum bright ring at a radius of 69 au and overlaps with the two millimeter continuum gaps at radii of 64 and 74 au. On the contrary, the presence of the central cavity is likely due to the high optical depth of the 3 mm continuum emission and not the depletion of the HCO+ gas. We derived the HCO+ column density profile from its intensity profile. From the column density profile, the FWHM widths of the inner and outer HCO+ gaps are both estimated to be ∼14 au, and their depths are estimated to be ∼2.4 and ∼5.0. These results are consistent with the expectation from the gaps opened by forming (sub-)Jovian mass planets, while placing tight constraints on the theoretical models solely incorporating the variation of dust properties and grain sizes.