Large-scale CO Spiral Arms and Complex Kinematics Associated with the T Tauri Star RU Lup

Large-scale CO Spiral Arms and Complex Kinematics Associated with the T Tauri Star RU Lup
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DOI:
10.3847/1538-4357/aba1e1
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发表时间:
2020-07
期刊:
The Astrophysical Journal
影响因子:
--
通讯作者:
Jane Huang;S. Andrews;K. Öberg;M. Ansdell;M. Benisty;J. Carpenter;A. Isella;L. P'erez;L. Ricci
Jane Huang;S. Andrews;K. Öberg;M. Ansdell;M. Benisty;J. Carpenter;A. Isella;L. P'erez;L. Ricci
中科院分区:
其他
文献类型:
--
作者:
Jane Huang;S. Andrews;K. Öberg;M. Ansdell;M. Benisty;J. Carpenter;A. Isella;L. P'erez;L. Ricci

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虽然原行星盘在毫米连续发射中通常看起来很紧凑,组织良好,但CO谱线观测越来越多地揭示了距离主星很远的复杂行为。我们展示了12CO、13CO和C18O的J = 2−1跃迁的深阿塔卡马大毫米/亚毫米阵列图,以及DCO+的J = 3−2跃迁,朝向金牛座T星RU Lup,分辨率为0.3″(~ 50 au)。CO同位素发射追踪了RU Lup系统的四个主要组成部分:一个半径为~ 120 au的紧凑的开普勒圆盘,一个围绕着圆盘的非开普勒“包膜状”结构,延伸到距恒星约260 au的地方,至少有五个延伸到1000 au的蓝移螺旋臂,以及从RU Lup投射到1500 au的螺旋臂外的团块。我们对RU - Lup奇特的气体形态的潜在解释进行了评论,包括引力不稳定性,物质吸积到磁盘上,或受到另一颗恒星的扰动。RU - Lup扩展的非开普勒CO排放,增加的恒星吸积率和不寻常的光度变化表明,它可能是爆发的FU - Ori系统的缩小的II类模拟物。
While protoplanetary disks often appear to be compact and well organized in millimeter continuum emission, CO spectral line observations are increasingly revealing complex behavior at large distances from the host star. We present deep Atacama Large Millimeter/submillimeter Array maps of the J = 2−1 transition of 12CO, 13CO, and C18O, as well as the J = 3−2 transition of DCO+, toward the T Tauri star RU Lup at a resolution of ∼0.3″ (∼50 au). The CO isotopologue emission traces four major components of the RU Lup system: a compact Keplerian disk with a radius of ∼120 au, a non-Keplerian “envelope-like” structure surrounding the disk and extending to ∼260 au from the star, at least five blueshifted spiral arms stretching up to 1000 au, and clumps outside the spiral arms located up to 1500 au in projection from RU Lup. We comment on potential explanations for RU Lup’s peculiar gas morphology, including gravitational instability, accretion of material onto the disk, or perturbation by another star. RU Lup’s extended non-Keplerian CO emission, elevated stellar accretion rate, and unusual photometric variability suggest that it could be a scaled-down Class II analog of the outbursting FU Ori systems.