在DS Tau圆盘的缺口中是否隐藏着一颗行星？
Is the gap in the DS Tau disc hiding a planet?
摘要：
最近使用阿塔卡马大型毫米波阵列（ALMA）进行的毫米波勘测揭示了以环和间隙为特征的原行星盘。对于这种环的起源，一个可能的解释是潮汐与一个看不见的行星伴星的相互作用。DS头周围的原行星盘显示了一个很大的差距在ALMA观测在1.3毫米。我们构建了一个流体动力学模型的尘埃连续观测ALMA假设所观察到的差距是由一个行星之间的雕刻和五个木星的质量。我们适合的形状的径向强度分布沿光盘主轴变化的行星质量，尘埃盘质量，和系统的演化时间。最佳拟合模型得到的行星与$M_{\rm p}=3.5\,M_{\rm Jup}$和光盘与$M_{\rm dust}= 9.6\cdot10^{-5}\,M_{\odot}$。从这个结果开始，我们还计算了气体运动学中行星的预期签名，如CO排放所示。我们发现，这样的签名（在一个“扭结”的形式在信道映射）可以观察到ALMA与速度分辨率之间的$0.2-0.5\,\rm{kms}^{-1}$和30和50 mas之间的光束大小。
英文摘要：
Recent mm-wavelength surveys performed with the Atacama Large Millimeter Array (ALMA) have revealed protoplanetary discs characterized by rings and gaps. A possible explanation for the origin of such rings is the tidal interaction with an unseen planetary companion. The protoplanetary disc around DS Tau shows a wide gap in the ALMA observation at 1.3 mm. We construct a hydrodynamical model for the dust continuum observed by ALMA assuming the observed gap is carved by a planet between one and five Jupiter masses. We fit the shape of the radial intensity profile along the disc major axis varying the planet mass, the dust disc mass, and the evolution time of the system. The best fitting model is obtained for a planet with $M_{\rm p}=3.5\,M_{\rm Jup}$ and a disc with $M_{\rm dust}= 9.6\cdot10^{-5}\,M_{\odot}$. Starting from this result, we also compute the expected signature of the planet in the gas kinematics, as traced by CO emission. We find that such a signature (in the form of a "kink" in the channel maps) could be observed by ALMA with a velocity resolution between $0.2-0.5\,\rm{kms}^{-1}$ and a beam size between 30 and 50 mas.
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