论文标题
DS Tau圆盘中的缝隙是否隐藏了行星？
Is the gap in the DS Tau disc hiding a planet?
论文作者
论文摘要
最近用Atacama大毫米阵列（ALMA）进行的MM波长调查表明，原电磁盘以环和间隙为特征。对这种环的起源的可能解释是与看不见的行星伴侣的潮汐相互作用。 DS tau周围的原球盘在1.3 mm处显示出Alma观察的较大差距。假设观察到的间隙是由一个和五个木星质量之间的行星雕刻的，我们为阿尔玛观察到的尘埃连续体构建了一个流体动力学模型。我们沿着圆盘的主要轴拟合了径向强度曲线的形状，这些轴轴，使行星质量，灰尘盘质量和系统的演变时间变化。最佳拟合模型是为具有$ M _ {\ rm P} = 3.5 \，M _ {\ rm jup} $的行星获得的，以及带有$ M _ {\ rm dust} = 9.6 \ cdot10^{ - 5} { - 5} \，m _ {\ odot} $的光盘。从此结果开始，我们还计算了通过CO发射所追踪的气体运动学中行星的预期特征。我们发现，Alma可以观察到这样的签名（以通道图中的“扭结”形式），速度分辨率在$ 0.2-0.5 \，\ rm {kms}^{ - 1} $和梁大小之间的速度分辨率之间。
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.
