论文标题
Alma观察到SZ周围的原星磁盘中的内腔84
ALMA Observations of the Inner Cavity in the Protoplanetary Disk around Sz 84
论文作者
论文摘要
我们介绍了大型毫米/亚毫米阵列（ALMA）观察到T Tauri Star SZ〜84周围的原球盘以及对灰尘磁盘中部内部腔内结构的分析。已知SZ〜84的光谱能量分布（SED）在$λ\ Lessim $ 10〜 $μ$ m上表现出可忽略的红外过量，这是由于磁盘的腔体结构。对观察到的灰尘连续性在1.3毫米处的可见性的分析表明，大（毫米尺寸）灰尘晶粒的磁盘的大小在半径上为8〜AU，而在小（亚微米尺寸）的圆盘中，半径为60 〜AU，半径为60〜AU。此外，从SED分析中，我们估计，小粉尘的上限质量$ r <$ 60〜AU小于$ \ sim $ 10 $ 10 $^{ - 3} $〜$〜$〜$ m _ {\ rm Earth} $，是$ \ lisssim $ 0.01〜 $ 0.01〜 \ $ 0.01〜 \ $ 0.01〜 $ 0.01〜 $ $+$+$+$+$ y $ y $ y $这些结果表明，大型尘土颗粒在$ r <$ 60〜AU上占主导地位，这意味着在该区域中，粉尘谷物在该区域有效地生长较低，这可能是由于湍流弱和/或粘稠的灰尘晶粒所致。晶粒生长和灰尘碎片化的平衡是确定原球门磁盘中大灰尘晶粒大小的重要因素，因此SZ〜84可以作为研究此类磁盘中谷物生长的良好测试。
We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of a protoplanetary disk around the T Tauri star Sz~84 and analyses of the structures of the inner cavity in the central region of the dust disk. Sz~84's spectral energy distribution (SED) has been known to exhibit negligible infrared excess at $λ\lesssim$10~$μ$m due to the disk's cavity structure. Analyses of the observed visibilities of dust continuum at 1.3~mm and the SED indicate that the size of the cavity in the disk of large (millimeter size) dust grains is 8~au in radius and that in the disk of small (sub-micron size) dust grains is 60~au in radius. Furthermore, from the SED analyses, we estimate that the upper limit mass of small dust grains at $r<$60~au is less than $\sim$10$^{-3}$~$M_{\rm earth}$, which is $\lesssim$0.01~\% of the total (small~$+$~large) dust mass at $r<$60~au. These results suggest that large dust grains are dominant at $r<$60~au, implying that dust grains efficiently grow with less efficient fragmentation in this region, potentially due to weak turbulence and/or stickier dust grains. The balance of grain growth and dust fragmentation is an important factor for determining the size of large dust grains in protoplanetary disks, and thus Sz~84 could serve as a good testbed for investigations of grain growth in such disks.
