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arXiv 0903.4455astro-ph.SRastro-ph.EP
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御夫座GM盘的空间分辨内孔

A Spatially Resolved Inner Hole in the Disk around GM Aurigae

A. Meredith Hughes, Sean M. Andrews, Catherine Espaillat, David J. Wilner, Nuria Calvet, Paola D'Alessio, Chunhua Qi, Jonathan P. Williams, Michiel Hogerheijde

备注：
12 pages, 6 figures, accepted for publication in ApJ
发表信息：
Astrophys.J.698:131-142,2009
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摘要：

我们提出了0.3弧秒分辨率的观测GM御夫座周围的磁盘与亚毫米阵列（SMA）在860微米的波长和高原德布尔干涉仪在1.3毫米的波长。这些观测探测磁盘材料的分布在空间尺度上相称的内孔的大小预测的光谱能量分布模型。这些数据清楚地表明，在盘中心的毫米光学深度急剧下降，与距离恒星不到20 AU的物质赤字相一致。我们改进的吸积盘模型。（2005年）的基础上未解决的光谱能量分布（SED），并证明它再现了空间分辨毫米连续谱数据在两个可用的波长。我们还提出了补充SMA观测的CO J=3-2和J=2-1从磁盘在2”的分辨率。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;以及（2）运动学旋转模式的位置角与在更小尺度上从尘埃连续体测量的位置角相差11 +/-2度，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。

英文摘要：

We present 0.3 arcsec resolution observations of the disk around GM Aurigae with the Submillimeter Array (SMA) at a wavelength of 860 um 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. 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. (2005) based on the unresolved spectral energy distribution (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 degrees 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.

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