A SPATIALLY RESOLVED INNER HOLE IN THE DISK AROUND GM AURIGAE
A SPATIALLY RESOLVED INNER HOLE IN THE DISK AROUND GM AURIGAE
复制标题
GM AURIGAE 周围圆盘上的空间解析内孔
DOI：
10.1088/0004-637x/698/1/131
复制
发表时间：
2009
期刊：
影响因子：
--
通讯作者：
M. Hogerheijde
中科院分区：
文献类型：
--
作者：
A. Hughes;S. Andrews;C. Espaillat;D. Wilner;N. Calvet;P. D’Alessio;C. Qi;Jonathan P. Williams;M. Hogerheijde
利用波长为860 μm的亚毫米波阵列（SMA）和波长为1.3 mm的Plateau de Bure干涉仪，对御夫座GM星周围的盘进行了0.“3分辨率的观测。这些观测结果探测了盘物质在空间尺度上的分布，与光谱能量分布（SED）模型预测的内孔大小相当。这些数据清楚地表明，在圆盘中心，毫米光学深度急剧下降，与距离星星不到20 Au的物质不足相一致。我们完善的吸积盘模型的Calvet等人。未解决的SED的基础上，并证明它再现空间分辨毫米连续谱数据在两个可用的波长。我们还提供了2″分辨率下的补充SMA观测结果，即来自盘的CO J = 3-2和J = 2-1发射。观测到的CO形态与连续介质模型的预测相一致，但有两个显著的偏差：（1）COJ = 3-2/J = 2-1的线比比大于预测值，这可能表明盘上层气体的额外加热;（2）运动学旋转模式的位置角与尘埃连续体小尺度测量的位置角相差11° ± 2°，这可以指示翘曲的存在。我们注意到，光蒸发，晶粒生长，和二元性是不太可能的机制诱导观察到的急剧下降的不透明度或表面密度在磁盘中心。内洞可能是行星对圆盘物质的动力学影响的结果。由行星引起的弯曲也可能解释连续体和CO数据集之间的位置角差异。
We present 0.″3 resolution observations of the disk around GM Aurigae with the Submillimeter Array (SMA) at a wavelength of 860 μm and with the Plateau de Bure Interferometer at a wavelength of 1.3 mm. These observations probe the distribution of disk material on spatial scales commensurate with the size of the inner hole predicted by models of the spectral energy distribution (SED). The data clearly indicate a sharp decrease in millimeter optical depth at the disk center, consistent with a deficit of material at distances less than ∼20 AU from the star. We refine the accretion disk model of Calvet et al. based on the unresolved SED and demonstrate that it reproduces well the spatially resolved millimeter continuum data at both available wavelengths. We also present complementary SMA observations of CO J = 3–2 and J = 2–1 emission from the disk at 2″ resolution. The observed CO morphology is consistent with the continuum model prediction, with two significant deviations: (1) the emission displays a larger CO J = 3–2/J = 2–1 line ratio than predicted, which may indicate additional heating of gas in the upper disk layers; and (2) the position angle of the kinematic rotation pattern differs by 11° ± 2° from that measured at smaller scales from the dust continuum, which may indicate the presence of a warp. We note that photoevaporation, grain growth, and binarity are unlikely mechanisms for inducing the observed sharp decrease in opacity or surface density at the disk center. The inner hole plausibly results from the dynamical influence of a planet on the disk material. Warping induced by a planet could also potentially explain the difference in position angle between the continuum and CO data sets.