论文标题
与Alma的行星腰带的调查：周围检测到的气体围绕太阳般的恒星HD 129590
Survey of planetesimal belts with ALMA: gas detected around the Sun-like star HD 129590
论文作者
论文摘要
围绕主要序列恒星的气体检测越来越普遍，大约有20个系统显示CO的存在。但是，需要更多的检测，尤其是在以后的光谱型恒星附近，以更好地了解这种气体的起源并完善我们的模型。为此，我们对10颗恒星进行了一项调查，该恒星使用ALMA在Band 6中进行了预测的次级CO检测的高可能性。我们寻找MM-DUST和气体发射的连续发射（CO和CN跃迁）。在9/10个系统中检测到了连续排放，我们为其得出了圆盘的尘埃质量和几何特性，提供了第一个毫米波检测到HD 106906，这是HD 106906，这是HD 114082、117214，HD 15745，HD 191089的第一个MM-Wave Radius，您在HD 191089和HD 191089和HD 191089和所有HD中均为HD 1211。与我们的早期太阳相似，这是第一次在年轻的10-16 Myr G1V Star HD 129590附近检测CO。气体似乎与行星腰带的同时存在，总质量可能在$ 2-10 \ times 10^{-5} $ m $ _ \ oplus $之间。围绕G型主序列恒星的第一次气体检测引发了有关是否在太阳系中也可能在其年轻人中释放气体的问题，这可能会影响星球的形成。我们还以比以前更高的S/N检测到HD 121191周围的CO气体，发现CO比系统中的行星更近得多，这可以证明这是先前怀疑的CO粘性散布，原因是由于屏蔽而阻止了其光电发射。最后，我们对行星中的CO含量和HCN/CO超出率（从CN上限）进行估计，我们发现这低于某些系统中太阳系彗星中看到的水平。
Gas detection around main sequence stars is becoming more common with around 20 systems showing the presence of CO. However, more detections are needed, especially around later spectral type stars to better understand the origin of this gas and refine our models. To do so, we carried out a survey of 10 stars with predicted high likelihoods of secondary CO detection using ALMA in band 6. We looked for continuum emission of mm-dust as well as gas emission (CO and CN transitions). The continuum emission was detected in 9/10 systems for which we derived the discs' dust masses and geometrical properties, providing the first mm-wave detection of the disc around HD 106906, the first mm-wave radius for HD 114082, 117214, HD 15745, HD 191089 and the first radius at all for HD 121191. A crucial finding of our paper is that we detect CO for the first time around the young 10-16 Myr old G1V star HD 129590, similar to our early Sun. The gas seems colocated with its planetesimal belt and its total mass is likely between $2-10 \times 10^{-5}$ M$_\oplus$. This first gas detection around a G-type main-sequence star raises questions as to whether gas may have been released in the Solar System as well in its youth, which could potentially have affected planet formation. We also detected CO gas around HD 121191 at a higher S/N than previously and find that the CO lies much closer-in than the planetesimals in the system, which could be evidence for the previously suspected CO viscous spreading owing to shielding preventing its photodissociation. Finally, we make estimates for the CO content in planetesimals and the HCN/CO outgassing rate (from CN upper limits), which we find are below the level seen in Solar System comets in some systems.
