Water in Protoplanetary Disks
Water in Protoplanetary Disks
复制标题
DOI：
10.1017/s1743921313012891
复制
发表时间：
2012-08
期刊：
影响因子：
--
通讯作者：
H. Nomura;C. Walsh;D. Heinzeller;T. Millar
中科院分区：
文献类型：
--
作者：
H. Nomura;C. Walsh;D. Heinzeller;T. Millar
摘要 最近由斯皮策和赫歇尔太空望远镜观测到的原行星盘的红外水线发射被认为追踪了盘内到外区域的表面层。我们对水丰度分布和线排放进行了建模，特别关注灰尘尺寸增长和湍流混合的影响。模型计算和观察之间的比较表明，具有湍流混合的小颗粒模型是首选。
Abstract Infrared water line emission from protoplanetary disks, recently observed by the Spitzer and Herschel space telescopes, is thought to trace the surface layer of the inner to outer regions of the disks. We have modelled the water abundance profile and line emission, especially focusing on the effects of dust size growth and turbulent mixing. Comparison between model calculations and observations suggests a small grain model with turbulent mixing is preferred.