论文标题
AU MIC的大兄弟姐妹：CP-72 2713周围的冷尘垃圾盘，$β$ PIC移动组
The big sibling of AU Mic: a cold dust-rich debris disk around CP-72 2713 in the $β$ Pic moving group
论文作者
论文摘要
分析Spitzer和Herschel档案测量结果，我们确定了围绕年轻的K7/M0星CP-72 2713的碎屑盘。该系统属于24myr Old $β$ PIC移动组。我们使用ALMA 7-M阵列获得的新的1.33毫米连续观测显示，伸展的灰尘盘，峰值半径为140AU，可能会追踪系统中行星皮带的位置。与已知的空间分辨碎片盘以及与类似质量的恒星周围的原月球盘相比，该磁盘非常大。发现该半径处的皮带的动态激发与行星搅拌可以对帐，而嵌入皮带中的大行星自动刺激只有在这些物体非常快速形成时才能起作用，例如通过卵石浓度。通过分析光谱能分布，我们得出了43K的特征性灰尘温度，而分数发光度为1.1 $ \ times $ 10 $^{ - 3} $。后一个值显着高，我们只知道在太阳40％以内的其他四个类似的灰尘富含粉尘的kuiper belt类似物。
Analyzing Spitzer and Herschel archival measurements we identified a debris disk around the young K7/M0 star CP-72 2713. The system belongs to the 24Myr old $β$ Pic moving group. Our new 1.33mm continuum observation, obtained with the ALMA 7-m array, revealed an extended dust disk with a peak radius of 140au, probably tracing the location of the planetesimal belt in the system. The disk is outstandingly large compared to known spatially resolved debris disks and also to protoplanetary disks around stars of comparable masses. The dynamical excitation of the belt at this radius is found to be reconcilable with planetary stirring, while self-stirring by large planetesimals embedded in the belt can work only if these bodies form very rapidly, e.g. via pebble concentration. By analyzing the spectral energy distribution we derived a characteristic dust temperature of 43K and a fractional luminosity of 1.1$\times$10$^{-3}$. The latter value is prominently high, we know only four other similarly dust-rich Kuiper-belt analogs within 40pc of the Sun.
