The Disk Substructures at High Angular Resolution Project (DSHARP). III. Spiral Structures in the Millimeter Continuum of the Elias 27, IM Lup, and WaOph 6 Disks
The Disk Substructures at High Angular Resolution Project (DSHARP). III. Spiral Structures in the Millimeter Continuum of the Elias 27, IM Lup, and WaOph 6 Disks
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DOI：
10.3847/2041-8213/aaf7a0
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发表时间：
2018-12
期刊：
影响因子：
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通讯作者：
Jane Huang;S. Andrews;L. P'erez;Zhaohuan Zhu;C. Dullemond;A. Isella;M. Benisty;M. Benisty;
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文献类型：
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作者：
Jane Huang;S. Andrews;L. P'erez;Zhaohuan Zhu;C. Dullemond;A. Isella;M. Benisty;M. Benisty;
我们提出了一个分析阿塔卡马大型毫米/亚毫米阵列1.25毫米连续观测的螺旋结构在三个原行星盘的磁盘子结构在高角分辨率项目。在Elias 27、IM Lup和WaOph 6周围的盘状物的分辨率为1040 - 60 mas（106 - 7 Au）。所有三个磁盘功能m = 2螺旋模式结合环形子结构。由12CO J = 2 − 1观测建立的气体运动学表明，连续谱旋臂是拖尾的。臂间强度对比适中，通常小于3。埃利亚斯27的螺旋图案延伸到整个磁盘的大部分，和武器相交的差距在R 69 Au。IM Lup盘中的螺旋图案特别复杂-它径向地延伸通过盘的大约一半，表现出螺距角随半径和臂间特征的变化，所述臂间特征可能是环子结构或螺旋臂分支的一部分。螺旋臂也延伸通过WaOph 6磁盘的大部分方式，但源整体上比其他两个磁盘更紧凑。我们讨论了螺旋结构的可能起源，包括引力不稳定性和密度波引起的恒星或行星的同伴。与许多在散射光中检测到的具有螺旋臂的盘的毫米连续对应物不同，这三个源不具有高对比度的新月状不对称性或大（R> 20 Au）发射腔。这种差异可能指向在盘中操作的多个螺旋形成机制。
We present an analysis of Atacama Large Millimeter/submillimeter Array 1.25 mm continuum observations of spiral structures in three protoplanetary disks from the Disk Substructures at High Angular Resolution Project. The disks around Elias 27, IM Lup, and WaOph 6 were observed at a resolution of ∼40–60 mas (∼6–7 au). All three disks feature m = 2 spiral patterns in conjunction with annular substructures. Gas kinematics established by 12CO J = 2−1 observations indicate that the continuum spiral arms are trailing. The arm–interarm intensity contrasts are modest, typically less than 3. The Elias 27 spiral pattern extends throughout much of the disk, and the arms intersect the gap at R ∼ 69 au. The spiral pattern in the IM Lup disk is particularly complex—it extends about halfway radially through the disk, exhibiting pitch angle variations with radius and interarm features that may be part of ring substructures or spiral arm branches. Spiral arms also extend most of the way through the WaOph 6 disk, but the source overall is much more compact than the other two disks. We discuss possible origins for the spiral structures, including gravitational instability and density waves induced by a stellar or planetary companion. Unlike the millimeter continuum counterparts of many of the disks with spiral arms detected in scattered light, these three sources do not feature high-contrast crescent-like asymmetries or large (R > 20 au) emission cavities. This difference may point to multiple spiral formation mechanisms operating in disks.