Tracing large-scale structures in circumstellar disks with ALMA
Tracing large-scale structures in circumstellar disks with ALMA
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DOI：
10.1051/0004-6361/201220390
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发表时间：
2012-12
影响因子：
6.5
通讯作者：
J. P. Ruge;S. Wolf;A. Uribe;H. Klahr
中科院分区：
文献类型：
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作者：
J. P. Ruge;S. Wolf;A. Uribe;H. Klahr
语境。行星应该是在星周盘中形成的。行星的额外引力势会扰动圆盘，并导致圆盘密度剖面中出现特征结构，即螺旋波和间隙。目标。我们对阿塔卡马大型（亚）毫米阵列（ALMA）在（亚）毫米波长范围内的星周盘中这些行星引起的结构的可观测性进行了大规模参数研究。方法。在星-盘-行星模型的流体动力学和磁流体动力学模拟的基础上，我们计算了这些系统的盘温度结构和（亚）毫米图像。这些用于导出模拟 ALMA 图像。因为合适的天体在金牛座-御夫座区域很常见，所以我们关注的距离为 140 pc，赤纬为 ≈20°。探索的星-盘-行星构型范围包括 6 个流体动力学模拟（包括磁场和不同的行星质量）、9 个外半径范围为 9 AU 到 225 AU 的盘尺寸、15 个总盘质量在 2.67 × 10 -7 之间的范围。 M� 和 4.10 × 10 -2 M� ，六颗不同的中心恒星，以及两种不同的晶粒尺寸分布，产生了 10 000 个圆盘模型。
Context. Planets are supposed to form in circumstellar disks. The additional gravitational potential of a planet perturbs the disk and leads to characteristic structures, i.e. spiral waves and gaps, in the disk’s density profile. Aims. We perform a large-scale parameter study of the observability of these planet-induced structures in circumstellar disks in the (sub)mm wavelength range for the Atacama Large (Sub)Millimeter Array (ALMA). Methods. On the basis of hydrodynamical and magneto-hydrodynamical simulations of star-disk-planet models, we calculated the disk temperature structure and (sub)mm images of these systems. These were used to derive simulated ALMA images. Because appropriate objects are frequent in the Taurus-Auriga region, we focused on a distance of 140 pc and a declination of ≈20 ◦ .T he explored range of star-disk-planet configurations consists of six hydrodynamical simulations (including magnetic fields and different planet masses), nine disk sizes with outer radii ranging from 9 AU to 225 AU, 15 total disk masses in the range between 2.67 × 10 −7 M� and 4.10 × 10 −2 M� ,s ix different central stars, and two different grain size distributions, resulting in 10 000 disk models.