The Detection of Dust Gap-ring Structure in the Outer Region of the CR Cha Protoplanetary Disk
The Detection of Dust Gap-ring Structure in the Outer Region of the CR Cha Protoplanetary Disk
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DOI：
10.3847/1538-4357/ab5d2b
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发表时间：
2019-11
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影响因子：
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通讯作者：
Seongjoong Kim;Sanemichi Z. Takahashi;H. Nomura;T. Tsukagoshi;Seokho Lee;T. Muto;R. Dong;Y. Hasegawa
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文献类型：
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作者：
Seongjoong Kim;Sanemichi Z. Takahashi;H. Nomura;T. Tsukagoshi;Seokho Lee;T. Muto;R. Dong;Y. Hasegawa
我们观察尘埃连续体在225 GHz和CO同位素（12 CO，13 CO和C18 O）J = 2-1发射线对CR查原行星盘使用阿塔卡马大型毫米/亚毫米阵列。尘埃连续体图像显示了尘埃盘外部区域的尘埃间隙环结构。在尘埃间隙之外的120 Au附近还探测到一个微弱的尘埃环。CO同位素谱线表明气体盘比尘埃盘更长。13 CO谱线的峰值亮度温度在130 Au附近有一个小的凸起，而12 CO谱线则没有。我们研究了两种可能的机制再现所观察到的尘埃间隙环结构和气体温度颠簸。首先，利用行星质量与差距深度和宽度之间的关系，可以通过一颗质量为1000亿的行星打开观测到的间隙结构。同时，基于观测到的尘埃表面密度分布的辐射传输计算表明，观测到的尘埃环可能是由尘埃在尘埃盘外缘外产生的气体温包，即气体压包处的积累形成的。
We observe the dust continuum at 225 GHz and CO isotopologue (12CO, 13CO, and C18O) J = 2–1 emission lines toward the CR Cha protoplanetary disk using the Atacama Large Millimeter/submillimeter Array. The dust continuum image shows a dust gap-ring structure in the outer region of the dust disk. A faint dust ring is also detected around 120 au beyond the dust gap. The CO isotopologue lines indicate that the gas disk is more extended than the dust disk. The peak brightness temperature of the 13CO line shows a small bump around 130 au, while 12CO lines do not. We investigate two possible mechanisms for reproducing the observed dust gap-ring structure and a gas temperature bump. First, the observed gap structure can be opened by a Jupiter-mass planet using the relation between the planet mass and the gap depth and width. Meanwhile, the radiative transfer calculations based on the observed dust surface density profile show that the observed dust ring could be formed by dust accumulation at the gas temperature bump, that is, the gas pressure bump produced beyond the outer edge of the dust disk.